Y |
Name | Schema Table | Database | Description | Type | Length | Unit | Default Value | Unified Content Descriptor |
y |
allwise_sc |
WISE |
Unit sphere position y value |
float |
8 |
|
|
|
y |
combo17CDFSSource |
COMBO17 |
y-coordinate on image cdfs_r.fit |
real |
4 |
pix |
|
|
y |
sharksDetection |
SHARKSv20210222 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
sharksDetection |
SHARKSv20210421 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
smashdr2_source |
SMASH |
Y-coordinate for this source in the original chip (1-indexed) |
real |
4 |
|
|
|
y |
ultravistaDetection, ultravistaMapRemeasurement |
ULTRAVISTADR4 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSDR2 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSDR3 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSDR4 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSDR5 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSDR6 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20120926 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20130417 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20140409 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20150108 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20160114 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20160507 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20170630 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20180419 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection |
VHSv20201209 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vhsDetection, vhsListRemeasurement |
VHSDR1 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEODR2 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEODR3 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEODR4 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEODR5 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEOv20100513 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoDetection |
VIDEOv20111208 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
videoListRemeasurement |
VIDEOv20100513 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGDR2 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGDR3 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGDR4 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20111019 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20130417 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20140402 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20150421 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20151230 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20160406 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20161202 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection |
VIKINGv20170715 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingDetection, vikingListRemeasurement |
VIKINGv20110714 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingMapRemeasurement |
VIKINGZYSELJv20160909 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vikingMapRemeasurement |
VIKINGZYSELJv20170124 |
Y coordinate of detection (SE: Y_IMAGE) {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCDR1 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCDR2 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCDR3 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCDR4 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCDR5 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20110909 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20120126 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20121128 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20130304 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20130805 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20140428 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20140903 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20150309 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20151218 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20160311 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20160822 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20170109 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20170411 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20171101 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20180702 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20181120 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20191212 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20210708 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection |
VMCv20230816 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcDetection, vmcListRemeasurement |
VMCv20110816 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vmcdeepDetection |
VMCDEEPv20230713 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vvvDetection |
VVVDR1 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vvvDetection |
VVVDR2 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles |
VVVDR5 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y |
vvvDetection, vvvListRemeasurement |
VVVv20100531 |
Y coordinate of detection {catalogue TType keyword: Y_coordinate} Intensity-weighted isophotal centre-of-gravity in Y. |
real |
4 |
pixels |
|
pos.cartesian.y;instr.plate |
y_1AperMag1 |
vvvSource |
VVVDR5 |
Point source Y_1 aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_1AperMag1Err |
vvvSource |
VVVDR5 |
Error in point source Y_1 mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_1AperMag3 |
vvvSource |
VVVDR5 |
Default point source Y_1 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_1AperMag3Err |
vvvSource |
VVVDR5 |
Error in default point source Y_1 mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_1AperMag4 |
vvvSource |
VVVDR5 |
Point source Y_1 aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_1AperMag4Err |
vvvSource |
VVVDR5 |
Error in point source Y_1 mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_1AverageConf |
vvvSource |
VVVDR5 |
average confidence in 2 arcsec diameter default aperture (aper3) Y_1 |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
y_1Class |
vvvSource |
VVVDR5 |
discrete image classification flag in Y_1 |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
y_1ClassStat |
vvvSource |
VVVDR5 |
S-Extractor classification statistic in Y_1 |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
y_1Ell |
vvvSource |
VVVDR5 |
1-b/a, where a/b=semi-major/minor axes in Y_1 |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
y_1eNum |
vvvMergeLog |
VVVDR5 |
the extension number of this Y_1 frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
y_1eNum |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the extension number of this 1st epoch Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
y_1ErrBits |
vvvSource |
VVVDR5 |
processing warning/error bitwise flags in Y_1 |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
y_1Eta |
vvvSource |
VVVDR5 |
Offset of Y_1 detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
y_1Gausig |
vvvSource |
VVVDR5 |
RMS of axes of ellipse fit in Y_1 |
real |
4 |
pixels |
-0.9999995e9 |
src.morph.param;em.IR.NIR |
y_1mfID |
vvvMergeLog |
VVVDR5 |
the UID of the relevant Y_1 multiframe |
bigint |
8 |
|
|
meta.id;obs.field;em.IR.NIR |
y_1mfID |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the UID of the relevant 1st epoch Y tile multiframe |
bigint |
8 |
|
|
meta.id;obs.field;em.IR.NIR |
y_1Mjd |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the MJD of the 1st epoch Y tile multiframe |
float |
8 |
|
|
time;em.IR.NIR |
y_1Mjd |
vvvSource |
VVVDR5 |
Modified Julian Day in Y_1 band |
float |
8 |
days |
-0.9999995e9 |
time.epoch;em.IR.NIR |
y_1PA |
vvvSource |
VVVDR5 |
ellipse fit celestial orientation in Y_1 |
real |
4 |
Degrees |
-0.9999995e9 |
pos.posAng;em.IR.NIR |
y_1ppErrBits |
vvvSource |
VVVDR5 |
additional WFAU post-processing error bits in Y_1 |
int |
4 |
|
0 |
meta.code;em.IR.NIR |
y_1SeqNum |
vvvSource |
VVVDR5 |
the running number of the Y_1 detection |
int |
4 |
|
-99999999 |
meta.number;em.IR.NIR |
y_1Xi |
vvvSource |
VVVDR5 |
Offset of Y_1 detection from master position (+east/-west) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.ra;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
y_2AperMag1 |
vvvSource |
VVVDR5 |
Point source Y_2 aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_2AperMag1Err |
vvvSource |
VVVDR5 |
Error in point source Y_2 mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_2AperMag3 |
vvvSource |
VVVDR5 |
Default point source Y_2 aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_2AperMag3Err |
vvvSource |
VVVDR5 |
Error in default point source Y_2 mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_2AperMag4 |
vvvSource |
VVVDR5 |
Point source Y_2 aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
y_2AperMag4Err |
vvvSource |
VVVDR5 |
Error in point source Y_2 mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
y_2AverageConf |
vvvSource |
VVVDR5 |
average confidence in 2 arcsec diameter default aperture (aper3) Y_2 |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
y_2Class |
vvvSource |
VVVDR5 |
discrete image classification flag in Y_2 |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
y_2ClassStat |
vvvSource |
VVVDR5 |
S-Extractor classification statistic in Y_2 |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
y_2Ell |
vvvSource |
VVVDR5 |
1-b/a, where a/b=semi-major/minor axes in Y_2 |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
y_2eNum |
vvvMergeLog |
VVVDR5 |
the extension number of this Y_2 frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
y_2eNum |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the extension number of this 2nd epoch Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
y_2ErrBits |
vvvSource |
VVVDR5 |
processing warning/error bitwise flags in Y_2 |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
y_2Eta |
vvvSource |
VVVDR5 |
Offset of Y_2 detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
y_2Gausig |
vvvSource |
VVVDR5 |
RMS of axes of ellipse fit in Y_2 |
real |
4 |
pixels |
-0.9999995e9 |
src.morph.param;em.IR.NIR |
y_2mfID |
vvvMergeLog |
VVVDR5 |
the UID of the relevant Y_2 multiframe |
bigint |
8 |
|
|
meta.id;obs.field;em.IR.NIR |
y_2mfID |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the UID of the relevant 2nd epoch Y tile multiframe |
bigint |
8 |
|
|
meta.id;obs.field;em.IR.NIR |
y_2Mjd |
vvvPsfDophotZYJHKsMergeLog |
VVVDR5 |
the MJD of the 2nd epoch Y tile multiframe |
float |
8 |
|
|
time;em.IR.NIR |
y_2Mjd |
vvvSource |
VVVDR5 |
Modified Julian Day in Y_2 band |
float |
8 |
days |
-0.9999995e9 |
time.epoch;em.IR.NIR |
y_2PA |
vvvSource |
VVVDR5 |
ellipse fit celestial orientation in Y_2 |
real |
4 |
Degrees |
-0.9999995e9 |
pos.posAng;em.IR.NIR |
y_2ppErrBits |
vvvSource |
VVVDR5 |
additional WFAU post-processing error bits in Y_2 |
int |
4 |
|
0 |
meta.code;em.IR.NIR |
y_2SeqNum |
vvvSource |
VVVDR5 |
the running number of the Y_2 detection |
int |
4 |
|
-99999999 |
meta.number;em.IR.NIR |
y_2Xi |
vvvSource |
VVVDR5 |
Offset of Y_2 detection from master position (+east/-west) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.ra;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
Y_BJ |
grs_ngpSource, grs_ranSource, grs_sgpSource |
TWODFGRS |
Plate y_bj in 8 micron pixels |
real |
4 |
|
|
|
y_coadd |
twomass_xsc |
TWOMASS |
y (in-scan) position (coadd coord.). |
real |
4 |
arcsec |
|
pos.cartesian;instr.det |
Y_IMAGE |
mgcDetection |
MGC |
Object y position |
real |
4 |
pixel |
|
|
Y_OFF |
mgcGalaxyStruct |
MGC |
Y offset of Galaxy Centre |
real |
4 |
|
99.99 |
|
Y_OFFm |
mgcGalaxyStruct |
MGC |
Y offset error (-) |
real |
4 |
|
99.99 |
|
Y_OFFp |
mgcGalaxyStruct |
MGC |
Y offset error (+) |
real |
4 |
|
99.99 |
|
Y_R |
spectra |
SIXDF |
y position of object from R frame |
int |
4 |
|
|
|
Y_V |
spectra |
SIXDF |
y position of object from V frame |
int |
4 |
|
|
|
yAmpl |
vmcCepheidVariables |
VMCDR4 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20160311 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20160822 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20170109 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20170411 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20171101 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20180702 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20181120 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20191212 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20210708 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmpl |
vmcCepheidVariables |
VMCv20230816 |
Peak-to-Peak amplitude in Y band {catalogue TType keyword: A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCDR4 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20160311 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20160822 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20170109 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20170411 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20171101 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20180702 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20181120 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20191212 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20210708 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAmplErr |
vmcCepheidVariables |
VMCv20230816 |
Error in Peak-to-Peak amplitude in Y band {catalogue TType keyword: e_A(Y)} |
real |
4 |
mag |
-0.9999995e9 |
stat.error;src.var.amplitude;em.IR.NIR |
yAperJky3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky3Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky4Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (2.8 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJky6Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJky6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (5.7 arcsec aperture diameter) calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
stat.error |
yAperJkyNoAperCorr3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux If in doubt use this flux estimator |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperJkyNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture calibrated flux |
real |
4 |
jansky |
-0.9999995e9 |
phot.flux |
yAperLup3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup3Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup4Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (2.8 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLup6Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLup6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (5.7 arcsec aperture diameter) luptitude |
real |
4 |
lup |
-0.9999995e9 |
stat.error |
yAperLupNoAperCorr3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture luptitude If in doubt use this flux estimator |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperLupNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture luptitude |
real |
4 |
lup |
-0.9999995e9 |
phot.lup |
yAperMag1 |
vmcSynopticSource |
VMCDR1 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCDR2 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCDR3 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCDR4 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCDR5 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20110816 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCv20110909 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCv20120126 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCv20121128 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCv20130304 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vmcSynopticSource |
VMCv20130805 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20140428 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20140903 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20150309 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20151218 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20160311 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20160822 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20170109 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20170411 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20171101 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20180702 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20181120 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20191212 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20210708 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vmcSynopticSource |
VMCv20230816 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vvvSource |
VVVDR1 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vvvSource |
VVVDR5 |
Point source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1 |
vvvSource |
VVVv20100531 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vvvSource |
VVVv20110718 |
Extended source Y aperture corrected mag (0.7 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag1 |
vvvSource, vvvSynopticSource |
VVVDR2 |
Extended source Y aperture corrected mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCDR1 |
Error in extended source Y mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCDR2 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCDR3 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag1Err |
vmcSynopticSource |
VMCDR4 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCDR5 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20110816 |
Error in extended source Y mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20110909 |
Error in extended source Y mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20120126 |
Error in extended source Y mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20121128 |
Error in extended source Y mag (0.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20130304 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20130805 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vmcSynopticSource |
VMCv20140428 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20140903 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag1Err |
vmcSynopticSource |
VMCv20150309 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag1Err |
vmcSynopticSource |
VMCv20151218 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20160311 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20160822 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20170109 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20170411 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20171101 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20180702 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20181120 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20191212 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20210708 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vmcSynopticSource |
VMCv20230816 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vvvSource |
VVVDR1 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vvvSource |
VVVDR5 |
Error in point source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag1Err |
vvvSource |
VVVv20100531 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vvvSource |
VVVv20110718 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag1Err |
vvvSource, vvvSynopticSource |
VVVDR2 |
Error in extended source Y mag (1.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2 |
vmcSynopticSource |
VMCDR1 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCDR2 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCDR3 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCDR4 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCDR5 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20110816 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCv20110909 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCv20120126 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCv20121128 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCv20130304 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vmcSynopticSource |
VMCv20130805 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20140428 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20140903 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20150309 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20151218 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20160311 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20160822 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20170109 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20170411 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20171101 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20180702 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20181120 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20191212 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20210708 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vmcSynopticSource |
VMCv20230816 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2 |
vvvSynopticSource |
VVVDR1 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag2 |
vvvSynopticSource |
VVVDR2 |
Extended source Y aperture corrected mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCDR1 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCDR2 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCDR3 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag2Err |
vmcSynopticSource |
VMCDR4 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCDR5 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20110816 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20110909 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20120126 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20121128 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20130304 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20130805 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vmcSynopticSource |
VMCv20140428 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20140903 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag2Err |
vmcSynopticSource |
VMCv20150309 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag2Err |
vmcSynopticSource |
VMCv20151218 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20160311 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20160822 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20170109 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20170411 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20171101 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20180702 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20181120 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20191212 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20210708 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vmcSynopticSource |
VMCv20230816 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag2Err |
vvvSynopticSource |
VVVDR1 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag2Err |
vvvSynopticSource |
VVVDR2 |
Error in extended source Y mag (1.4 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3 |
ultravistaSource |
ULTRAVISTADR4 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vhsSource |
VHSDR1 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vhsSource |
VHSDR2 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vhsSource |
VHSDR3 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSDR4 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSDR5 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSDR6 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20120926 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vhsSource |
VHSv20130417 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vhsSource |
VHSv20140409 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20150108 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20160114 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20160507 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20170630 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20180419 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vhsSource |
VHSv20201209 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
videoSource |
VIDEODR2 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
videoSource |
VIDEODR3 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
videoSource |
VIDEODR4 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
videoSource |
VIDEODR5 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
videoSource |
VIDEOv20100513 |
Default point/extended source Y mag, no aperture correction applied If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
videoSource |
VIDEOv20111208 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGDR2 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGDR3 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGDR4 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20110714 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGv20111019 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGv20130417 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingSource |
VIKINGv20140402 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20150421 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20151230 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20160406 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20161202 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingSource |
VIKINGv20170715 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default point source Y aperture corrected (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCDR1 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCDR2 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCDR3 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCDR4 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCDR5 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20110816 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCv20110909 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCv20120126 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCv20121128 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCv20130304 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSource |
VMCv20130805 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20140428 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20140903 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20150309 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20151218 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20160311 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20160822 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20170109 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20170411 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20171101 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20180702 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20181120 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20191212 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20210708 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSource |
VMCv20230816 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCDR1 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCDR2 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCDR3 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCDR4 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCDR5 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20110816 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCv20110909 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCv20120126 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCv20121128 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCv20130304 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vmcSynopticSource |
VMCv20130805 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20140428 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20140903 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20150309 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20151218 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20160311 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20160822 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20170109 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20170411 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20171101 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20180702 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20181120 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20191212 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20210708 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vmcSynopticSource |
VMCv20230816 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vvvSource |
VVVDR1 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vvvSource |
VVVDR2 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vvvSource |
VVVDR5 |
Default point source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vvvSource |
VVVv20100531 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vvvSource |
VVVv20110718 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vvvSynopticSource |
VVVDR1 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag3 |
vvvSynopticSource |
VVVDR2 |
Default point/extended source Y aperture corrected mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag3 |
vvvVivaCatalogue |
VVVDR5 |
Y magnitude using aperture corrected mag (2.0 arcsec aperture diameter, from VVVDR4 1st epoch ZY contemporaneous OB) {catalogue TType keyword: yAperMag3} |
real |
4 |
mag |
-9.999995e8 |
|
yAperMag3Err |
ultravistaSource |
ULTRAVISTADR4 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vhsSource |
VHSDR1 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vhsSource |
VHSDR2 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vhsSource |
VHSDR3 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSDR4 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vhsSource |
VHSDR5 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSDR6 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20120926 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vhsSource |
VHSv20130417 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vhsSource |
VHSv20140409 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20150108 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vhsSource |
VHSv20160114 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20160507 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20170630 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20180419 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vhsSource |
VHSv20201209 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
videoSource |
VIDEODR2 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
videoSource |
VIDEODR3 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
videoSource |
VIDEODR4 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
videoSource |
VIDEODR5 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
videoSource |
VIDEOv20100513 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
videoSource |
VIDEOv20111208 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGDR2 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGDR3 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGDR4 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag3Err |
vikingSource |
VIKINGv20110714 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGv20111019 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGv20130417 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGv20140402 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingSource |
VIKINGv20150421 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vikingSource |
VIKINGv20151230 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vikingSource |
VIKINGv20160406 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vikingSource |
VIKINGv20161202 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vikingSource |
VIKINGv20170715 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in default point/extended source Y (2.0 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCDR2 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCDR3 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vmcSource |
VMCDR4 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCDR5 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20110816 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20110909 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20120126 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20121128 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20130304 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20130805 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vmcSource |
VMCv20140428 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20140903 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vmcSource |
VMCv20150309 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag3Err |
vmcSource |
VMCv20151218 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20160311 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20160822 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20170109 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20170411 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20171101 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20180702 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20181120 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20191212 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20210708 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource |
VMCv20230816 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vmcSource, vmcSynopticSource |
VMCDR1 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vvvSource |
VVVDR2 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vvvSource |
VVVDR5 |
Error in default point source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag3Err |
vvvSource |
VVVv20100531 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vvvSource |
VVVv20110718 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vvvSource, vvvSynopticSource |
VVVDR1 |
Error in default point/extended source Y mag (2.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag3Err |
vvvVivaCatalogue |
VVVDR5 |
Error in default point source Y mag, from VVVDR4 {catalogue TType keyword: yAperMag3Err} |
real |
4 |
mag |
-9.999995e8 |
|
yAperMag4 |
ultravistaSource |
ULTRAVISTADR4 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vhsSource |
VHSDR1 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vhsSource |
VHSDR2 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vhsSource |
VHSDR3 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSDR4 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSDR5 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSDR6 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20120926 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vhsSource |
VHSv20130417 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vhsSource |
VHSv20140409 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20150108 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20160114 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20160507 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20170630 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20180419 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vhsSource |
VHSv20201209 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
videoSource |
VIDEODR2 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
videoSource |
VIDEODR3 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
videoSource |
VIDEODR4 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
videoSource |
VIDEODR5 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
videoSource |
VIDEOv20100513 |
Extended source Y mag, no aperture correction applied |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
videoSource |
VIDEOv20111208 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGDR2 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGDR3 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGDR4 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20110714 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGv20111019 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGv20130417 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingSource |
VIKINGv20140402 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20150421 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20151230 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20160406 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20161202 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingSource |
VIKINGv20170715 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCDR1 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCDR2 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCDR3 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCDR4 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCDR5 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20110816 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCv20110909 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCv20120126 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCv20121128 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCv20130304 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSource |
VMCv20130805 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20140428 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20140903 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20150309 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20151218 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20160311 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20160822 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20170109 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20170411 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20171101 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20180702 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20181120 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20191212 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20210708 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSource |
VMCv20230816 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCDR1 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCDR2 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCDR3 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCDR4 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCDR5 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20110816 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCv20110909 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCv20120126 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCv20121128 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCv20130304 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vmcSynopticSource |
VMCv20130805 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20140428 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20140903 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20150309 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20151218 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20160311 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20160822 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20170109 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20170411 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20171101 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20180702 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20181120 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20191212 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20210708 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vmcSynopticSource |
VMCv20230816 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vvvSource |
VVVDR2 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vvvSource |
VVVDR5 |
Point source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag4 |
vvvSource |
VVVv20100531 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vvvSource |
VVVv20110718 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4 |
vvvSource, vvvSynopticSource |
VVVDR1 |
Extended source Y aperture corrected mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag4Err |
ultravistaSource |
ULTRAVISTADR4 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (2.8 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vhsSource |
VHSDR1 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vhsSource |
VHSDR2 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vhsSource |
VHSDR3 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSDR4 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vhsSource |
VHSDR5 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSDR6 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20120926 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vhsSource |
VHSv20130417 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vhsSource |
VHSv20140409 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20150108 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vhsSource |
VHSv20160114 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20160507 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20170630 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20180419 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vhsSource |
VHSv20201209 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
videoSource |
VIDEODR2 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
videoSource |
VIDEODR3 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
videoSource |
VIDEODR4 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
videoSource |
VIDEODR5 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
videoSource |
VIDEOv20100513 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
videoSource |
VIDEOv20111208 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGDR2 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGDR3 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGDR4 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag4Err |
vikingSource |
VIKINGv20110714 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGv20111019 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGv20130417 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGv20140402 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingSource |
VIKINGv20150421 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vikingSource |
VIKINGv20151230 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vikingSource |
VIKINGv20160406 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vikingSource |
VIKINGv20161202 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vikingSource |
VIKINGv20170715 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (2.8 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (2.8 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCDR1 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCDR2 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCDR3 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSource |
VMCDR4 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCDR5 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20110816 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20110909 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20120126 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20121128 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20130304 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20130805 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSource |
VMCv20140428 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20140903 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSource |
VMCv20150309 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSource |
VMCv20151218 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20160311 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20160822 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20170109 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20170411 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20171101 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20180702 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20181120 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20191212 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20210708 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSource |
VMCv20230816 |
Error in point/extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCDR1 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCDR2 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCDR3 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSynopticSource |
VMCDR4 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCDR5 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20110816 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20110909 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20120126 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20121128 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20130304 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20130805 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vmcSynopticSource |
VMCv20140428 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20140903 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSynopticSource |
VMCv20150309 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag4Err |
vmcSynopticSource |
VMCv20151218 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20160311 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20160822 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20170109 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20170411 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20171101 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20180702 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20181120 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20191212 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20210708 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vmcSynopticSource |
VMCv20230816 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vvvSource |
VVVDR2 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vvvSource |
VVVDR5 |
Error in point source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag4Err |
vvvSource |
VVVv20100531 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vvvSource |
VVVv20110718 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag4Err |
vvvSource, vvvSynopticSource |
VVVDR1 |
Error in extended source Y mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5 |
vmcSynopticSource |
VMCDR1 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCDR2 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCDR3 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCDR4 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCDR5 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20110816 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCv20110909 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCv20120126 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCv20121128 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCv20130304 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vmcSynopticSource |
VMCv20130805 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20140428 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20140903 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20150309 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20151218 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20160311 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20160822 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20170109 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20170411 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20171101 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20180702 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20181120 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20191212 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20210708 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vmcSynopticSource |
VMCv20230816 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5 |
vvvSynopticSource |
VVVDR1 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag5 |
vvvSynopticSource |
VVVDR2 |
Extended source Y aperture corrected mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCDR1 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCDR2 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCDR3 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag5Err |
vmcSynopticSource |
VMCDR4 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCDR5 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20110816 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20110909 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20120126 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20121128 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20130304 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20130805 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vmcSynopticSource |
VMCv20140428 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20140903 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag5Err |
vmcSynopticSource |
VMCv20150309 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag5Err |
vmcSynopticSource |
VMCv20151218 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20160311 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20160822 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20170109 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20170411 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20171101 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20180702 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20181120 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20191212 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20210708 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vmcSynopticSource |
VMCv20230816 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag5Err |
vvvSynopticSource |
VVVDR1 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag5Err |
vvvSynopticSource |
VVVDR2 |
Error in extended source Y mag (4.0 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6 |
ultravistaSource |
ULTRAVISTADR4 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vhsSource |
VHSDR1 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vhsSource |
VHSDR2 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vhsSource |
VHSDR3 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSDR4 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSDR5 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSDR6 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20120926 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vhsSource |
VHSv20130417 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vhsSource |
VHSv20140409 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20150108 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20160114 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20160507 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20170630 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20180419 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vhsSource |
VHSv20201209 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
videoSource |
VIDEODR2 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
videoSource |
VIDEODR3 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
videoSource |
VIDEODR4 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
videoSource |
VIDEODR5 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
videoSource |
VIDEOv20100513 |
Extended source Y mag, no aperture correction applied |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
videoSource |
VIDEOv20111208 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGDR2 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGDR3 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGDR4 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20110714 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGv20111019 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGv20130417 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingSource |
VIKINGv20140402 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20150421 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20151230 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20160406 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20161202 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingSource |
VIKINGv20170715 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Point source Y aperture corrected (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCDR1 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCDR2 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCDR3 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCDR4 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCDR5 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20110816 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCv20110909 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCv20120126 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCv20121128 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCv20130304 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMag6 |
vmcSource |
VMCv20130805 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20140428 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20140903 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20150309 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20151218 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20160311 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20160822 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20170109 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20170411 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20171101 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20180702 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20181120 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20191212 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20210708 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6 |
vmcSource |
VMCv20230816 |
Point source Y aperture corrected mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMag6Err |
ultravistaSource |
ULTRAVISTADR4 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Error in point/extended source Y (5.7 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vhsSource |
VHSDR1 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vhsSource |
VHSDR2 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vhsSource |
VHSDR3 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSDR4 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vhsSource |
VHSDR5 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSDR6 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20120926 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vhsSource |
VHSv20130417 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vhsSource |
VHSv20140409 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20150108 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vhsSource |
VHSv20160114 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20160507 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20170630 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20180419 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vhsSource |
VHSv20201209 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
videoSource |
VIDEODR2 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
videoSource |
VIDEODR3 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
videoSource |
VIDEODR4 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
videoSource |
VIDEODR5 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
videoSource |
VIDEOv20100513 |
Error in extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
videoSource |
VIDEOv20111208 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGDR2 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGDR3 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGDR4 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag6Err |
vikingSource |
VIKINGv20110714 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGv20111019 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGv20130417 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGv20140402 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingSource |
VIKINGv20150421 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vikingSource |
VIKINGv20151230 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vikingSource |
VIKINGv20160406 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vikingSource |
VIKINGv20161202 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vikingSource |
VIKINGv20170715 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Error in point/extended source Y (5.7 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Error in point/extended source Y (5.7 arcsec aperture diameter) magnitude |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCDR1 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCDR2 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCDR3 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vmcSource |
VMCDR4 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCDR5 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20110816 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20110909 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20120126 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20121128 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20130304 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20130805 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error |
yAperMag6Err |
vmcSource |
VMCv20140428 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20140903 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vmcSource |
VMCv20150309 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;em.IR.NIR;phot.mag |
yAperMag6Err |
vmcSource |
VMCv20151218 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20160311 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20160822 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20170109 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20170411 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20171101 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20180702 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20181120 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20191212 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20210708 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMag6Err |
vmcSource |
VMCv20230816 |
Error in point/extended source Y mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
stat.error;phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
ultravistaSource |
ULTRAVISTADR4 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR1 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR2 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR3 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR4 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR5 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSDR6 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20120926 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20130417 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20140409 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20150108 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20160114 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20160507 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20170630 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20180419 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vhsSource |
VHSv20201209 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
videoSource |
VIDEODR2 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
videoSource |
VIDEODR3 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
videoSource |
VIDEODR4 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
videoSource |
VIDEODR5 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
videoSource |
VIDEOv20111208 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGDR2 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGDR3 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGDR4 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20110714 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20111019 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20130417 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20140402 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20150421 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20151230 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20160406 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20161202 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingSource |
VIKINGv20170715 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Default extended source Y (2.0 arcsec aperture diameter, but no aperture correction applied) aperture magnitude If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCDR1 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCDR2 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCDR3 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCDR4 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCDR5 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20110816 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20110909 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20120126 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20121128 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20130304 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20130805 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20140428 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20140903 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20150309 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20151218 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20160311 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20160822 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20170109 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20170411 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20171101 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20180702 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20181120 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20191212 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20210708 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr3 |
vmcSource |
VMCv20230816 |
Default extended source Y aperture mag (2.0 arcsec aperture diameter) If in doubt use this flux estimator |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
ultravistaSource |
ULTRAVISTADR4 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR1 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR2 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR3 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR4 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR5 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSDR6 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20120926 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20130417 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20140409 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20150108 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20160114 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20160507 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20170630 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20180419 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vhsSource |
VHSv20201209 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
videoSource |
VIDEODR2 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
videoSource |
VIDEODR3 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
videoSource |
VIDEODR4 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
videoSource |
VIDEODR5 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
videoSource |
VIDEOv20111208 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGDR2 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGDR3 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGDR4 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20110714 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20111019 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20130417 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20140402 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20150421 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20151230 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20160406 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20161202 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingSource |
VIKINGv20170715 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (2.8 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCDR1 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCDR2 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCDR3 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCDR4 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCDR5 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20110816 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20110909 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20120126 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20121128 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20130304 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20130805 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20140428 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20140903 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20150309 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20151218 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20160311 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20160822 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20170109 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20170411 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20171101 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20180702 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20181120 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20191212 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20210708 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr4 |
vmcSource |
VMCv20230816 |
Extended source Y aperture mag (2.8 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
ultravistaSource |
ULTRAVISTADR4 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR1 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR2 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR3 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR4 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR5 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSDR6 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20120926 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20130417 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20140409 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20150108 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20160114 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20160507 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20170630 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20180419 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vhsSource |
VHSv20201209 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
videoSource |
VIDEODR2 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
videoSource |
VIDEODR3 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
videoSource |
VIDEODR4 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
videoSource |
VIDEODR5 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
videoSource |
VIDEOv20111208 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGDR2 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGDR3 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGDR4 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20110714 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20111019 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20130417 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20140402 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20150421 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20151230 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20160406 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20161202 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingSource |
VIKINGv20170715 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
Extended source Y (5.7 arcsec aperture diameter, but no aperture correction applied) aperture magnitude |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCDR1 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCDR2 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCDR3 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCDR4 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCDR5 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20110816 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20110909 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20120126 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20121128 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20130304 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20130805 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20140428 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20140903 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20150309 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20151218 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20160311 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20160822 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20170109 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20170411 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20171101 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20180702 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20181120 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20191212 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20210708 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yAperMagNoAperCorr6 |
vmcSource |
VMCv20230816 |
Extended source Y aperture mag (5.7 arcsec aperture diameter) |
real |
4 |
mag |
-0.9999995e9 |
phot.mag;em.IR.NIR |
yApFillFac |
StackObjectAttributes |
PS1DR2 |
Aperture fill factor from y filter stack detection. |
real |
4 |
|
-999 |
|
yApFlux |
StackObjectAttributes |
PS1DR2 |
Aperture flux from y filter stack detection. |
real |
4 |
Janskys |
-999 |
|
yApFluxErr |
StackObjectAttributes |
PS1DR2 |
Error in aperture flux from y filter stack detection. |
real |
4 |
Janskys |
-999 |
|
yApMag |
StackObjectThin |
PS1DR2 |
Aperture magnitude from y filter stack detection. |
real |
4 |
AB magnitudes |
-999 |
|
yApMagErr |
StackObjectThin |
PS1DR2 |
Error in aperture magnitude from y filter stack detection. |
real |
4 |
AB magnitudes |
-999 |
|
yApRadius |
StackObjectAttributes |
PS1DR2 |
Aperture radius for y filter stack detection. |
real |
4 |
arcsec |
-999 |
|
yaStratAst |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, a, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratAst |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
yaStratPht |
ultravistaMapLcVarFrameSetInfo |
ULTRAVISTADR4 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, a, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yaStratPht |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c0 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yAverageConf |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSDR1 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vhsSource |
VHSDR2 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vhsSource |
VHSDR3 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSDR4 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSDR5 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSDR6 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20120926 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20130417 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20140409 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20150108 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20160114 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20160507 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20170630 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20180419 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vhsSource |
VHSv20201209 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGDR2 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vikingSource |
VIKINGDR3 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGDR4 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20110714 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vikingSource |
VIKINGv20111019 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vikingSource |
VIKINGv20130417 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20140402 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20150421 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20151230 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20160406 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20161202 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingSource |
VIKINGv20170715 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCDR2 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCDR3 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCDR4 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCDR5 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20110816 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vmcSource |
VMCv20110909 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vmcSource |
VMCv20120126 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vmcSource |
VMCv20121128 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20130304 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20130805 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20140428 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20140903 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20150309 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20151218 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20160311 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20160822 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20170109 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20170411 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20171101 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20180702 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20181120 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20191212 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20210708 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource |
VMCv20230816 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vmcSource, vmcSynopticSource |
VMCDR1 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
meta.code |
yAverageConf |
vvvSource |
VVVDR2 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vvvSource |
VVVDR5 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-0.9999995e9 |
stat.likelihood;em.IR.NIR |
yAverageConf |
vvvSource, vvvSynopticSource |
VVVDR1 |
average confidence in 2 arcsec diameter default aperture (aper3) Y |
real |
4 |
|
-99999999 |
stat.likelihood;em.IR.NIR |
YB |
eros2LMCSource, eros2SMCSource, erosLMCSource, erosSMCSource |
EROS |
Y pixel coordinate on blue reference images relative to rebined reference images in [klmn] frame |
real |
4 |
|
|
|
ybestAper |
ultravistaMapLcVariability |
ULTRAVISTADR4 |
Best aperture (1-3) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
ultravistaVariability |
ULTRAVISTADR4 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEODR2 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEODR3 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEODR4 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEODR5 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEOv20100513 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
videoVariability |
VIDEOv20111208 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vikingVariability |
VIKINGv20110714 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCDR1 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCDR2 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCDR3 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCDR4 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCDR5 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20110816 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20110909 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20120126 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
|
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20121128 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20130304 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20130805 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20140428 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20140903 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20150309 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20151218 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20160311 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20160822 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20170109 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20170411 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20171101 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20180702 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20181120 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20191212 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20210708 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vmcVariability |
VMCv20230816 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybestAper |
vvvVariability |
VVVDR5 |
Best aperture (1-6) for photometric statistics in the Y band |
int |
4 |
|
-9999 |
meta.code.class;em.IR.NIR |
Aperture magnitude (1-6) which gives the lowest RMS for the object. All apertures have the appropriate aperture correction. This can give better values in crowded regions than aperMag3 (see Irwin et al. 2007, MNRAS, 375, 1449) |
ybStratAst |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, b, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratAst |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ybStratPht |
ultravistaMapLcVarFrameSetInfo |
ULTRAVISTADR4 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, b, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ybStratPht |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c1 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqAst |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEODR2 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEODR3 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEODR4 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEODR5 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEOv20100513 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
videoVarFrameSetInfo |
VIDEOv20111208 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCDR1 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCDR2 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCDR3 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCDR4 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCDR5 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20110816 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20110909 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20120126 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20121128 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20130304 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20130805 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20140428 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20140903 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20150309 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20151218 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20160311 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20160822 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20170109 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20170411 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20171101 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20180702 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20181120 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20191212 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20210708 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vmcVarFrameSetInfo |
VMCv20230816 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqAst |
vvvVarFrameSetInfo |
VVVDR5 |
Goodness of fit of Strateva function to astrometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ychiSqpd |
ultravistaMapLcVariability |
ULTRAVISTADR4 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
ultravistaVariability |
ULTRAVISTADR4 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEODR2 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEODR3 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2 |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEODR4 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEODR5 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEOv20100513 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
videoVariability |
VIDEOv20111208 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vikingVariability |
VIKINGv20110714 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCDR1 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCDR2 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2 |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCDR3 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCDR4 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCDR5 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20110816 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20110909 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20120126 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
|
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20121128 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2 |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20130304 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2 |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20130805 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2 |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20140428 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20140903 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20150309 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20151218 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20160311 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20160822 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20170109 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20170411 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20171101 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20180702 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20181120 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20191212 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20210708 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vmcVariability |
VMCv20230816 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqpd |
vvvVariability |
VVVDR5 |
Chi square (per degree of freedom) fit to data (mean and expected rms) |
real |
4 |
|
-0.9999995e9 |
stat.fit.chi2;em.IR.NIR |
The photometry is calculated for good observations in the best aperture. The mean, rms, median, median absolute deviation, minMag and maxMag are quite standard. The skewness is calculated as in Sesar et al. 2007, AJ, 134, 2236. The number of good detections that are more than 3 standard deviations can indicate a distribution with many outliers. In each frameset, the mean and rms are used to derive a fit to the expected rms as a function of magnitude. The parameters for the fit are stored in VarFrameSetInfo and the value for the source is in expRms. This is subtracted from the rms in quadrature to get the intrinsic rms: the variability of the object beyond the noise in the system. The chi-squared is calculated, assuming a non-variable object which has the noise from the expected-rms and mean calculated as above. The probVar statistic assumes a chi-squared distribution with the correct number of degrees of freedom. The varClass statistic is 1, if the probVar>0.9 and intrinsicRMS/expectedRMS>3. |
ychiSqPht |
ultravistaMapLcVarFrameSetInfo, ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEODR2 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEODR3 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEODR4 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEODR5 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEOv20100513 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
videoVarFrameSetInfo |
VIDEOv20111208 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCDR1 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCDR2 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCDR3 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCDR4 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCDR5 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20110816 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20110909 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20120126 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20121128 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20130304 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20130805 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20140428 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20140903 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20150309 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20151218 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20160311 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20160822 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20170109 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20170411 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20171101 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20180702 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20181120 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20191212 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20210708 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vmcVarFrameSetInfo |
VMCv20230816 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ychiSqPht |
vvvVarFrameSetInfo |
VVVDR5 |
Goodness of fit of Strateva function to photometric data in Y band |
real |
4 |
|
-0.9999995e9 |
stat.fit.goodness;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
Yclass |
vvvParallaxCatalogue, vvvProperMotionCatalogue |
VVVDR5 |
VVV DR4 Y morphological classification. 1 = galaxy,0 = noise,-1 = stellar,-2 = probably stellar,-3 = probable galaxy,-7 = bad pixel within 2" aperture,-9 = saturated {catalogue TType keyword: Yclass} |
int |
4 |
|
-99999999 |
|
yClass |
ultravistaSource |
ULTRAVISTADR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vhsSource |
VHSDR2 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vhsSource |
VHSDR3 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSDR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSDR5 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSDR6 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20120926 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vhsSource |
VHSv20130417 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vhsSource |
VHSv20140409 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20150108 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20160114 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20160507 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20170630 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20180419 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource |
VHSv20201209 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vhsSource, vhsSourceRemeasurement |
VHSDR1 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
videoSource |
VIDEODR2 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
videoSource |
VIDEODR3 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
videoSource |
VIDEODR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
videoSource |
VIDEODR5 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
videoSource |
VIDEOv20111208 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
videoSource, videoSourceRemeasurement |
VIDEOv20100513 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGDR2 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGDR3 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGDR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource |
VIKINGv20111019 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGv20130417 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGv20140402 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingSource |
VIKINGv20150421 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource |
VIKINGv20151230 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource |
VIKINGv20160406 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource |
VIKINGv20161202 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource |
VIKINGv20170715 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vikingSource, vikingSourceRemeasurement |
VIKINGv20110714 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCDR2 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCDR3 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCDR4 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCDR5 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20110909 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCv20120126 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCv20121128 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCv20130304 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCv20130805 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource |
VMCv20140428 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20140903 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20150309 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20151218 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20160311 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20160822 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20170109 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20170411 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20171101 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20180702 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20181120 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20191212 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20210708 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource |
VMCv20230816 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vmcSource, vmcSourceRemeasurement |
VMCv20110816 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vmcSource, vmcSynopticSource |
VMCDR1 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vvvSource |
VVVDR2 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vvvSource |
VVVDR5 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class;em.IR.NIR |
yClass |
vvvSource |
VVVv20110718 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vvvSource, vvvSourceRemeasurement |
VVVv20100531 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClass |
vvvSource, vvvSynopticSource |
VVVDR1 |
discrete image classification flag in Y |
smallint |
2 |
|
-9999 |
src.class |
yClassStat |
ultravistaSource |
ULTRAVISTADR4 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vhsSource |
VHSDR2 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vhsSource |
VHSDR3 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSDR4 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSDR5 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSDR6 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20120926 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vhsSource |
VHSv20130417 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vhsSource |
VHSv20140409 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20150108 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20160114 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20160507 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20170630 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20180419 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource |
VHSv20201209 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vhsSource, vhsSourceRemeasurement |
VHSDR1 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
videoSource |
VIDEODR2 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
videoSource |
VIDEODR3 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
videoSource |
VIDEODR4 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
videoSource |
VIDEODR5 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
videoSource |
VIDEOv20100513 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
videoSource |
VIDEOv20111208 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
videoSourceRemeasurement |
VIDEOv20100513 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGDR2 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGDR3 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGDR4 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource |
VIKINGv20111019 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGv20130417 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGv20140402 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingSource |
VIKINGv20150421 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource |
VIKINGv20151230 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource |
VIKINGv20160406 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource |
VIKINGv20161202 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource |
VIKINGv20170715 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vikingSource, vikingSourceRemeasurement |
VIKINGv20110714 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCDR2 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCDR3 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCDR4 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCDR5 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20110909 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCv20120126 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCv20121128 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCv20130304 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCv20130805 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource |
VMCv20140428 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20140903 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20150309 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20151218 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20160311 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20160822 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20170109 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20170411 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20171101 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20180702 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20181120 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20191212 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20210708 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource |
VMCv20230816 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vmcSource, vmcSourceRemeasurement |
VMCv20110816 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vmcSource, vmcSynopticSource |
VMCDR1 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSource |
VVVDR1 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSource |
VVVDR2 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSource |
VVVDR5 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat;em.IR.NIR |
yClassStat |
vvvSource |
VVVv20100531 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSource |
VVVv20110718 |
S-Extractor classification statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSourceRemeasurement |
VVVv20100531 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSourceRemeasurement |
VVVv20110718 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSynopticSource |
VVVDR1 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
yClassStat |
vvvSynopticSource |
VVVDR2 |
N(0,1) stellarness-of-profile statistic in Y |
real |
4 |
|
-0.9999995e9 |
stat |
ycStratAst |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, c, in fit to astrometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratAst |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to astrometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS position around the mean for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. |
ycStratPht |
ultravistaMapLcVarFrameSetInfo |
ULTRAVISTADR4 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
ultravistaVarFrameSetInfo |
ULTRAVISTADR4 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEODR2 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEODR3 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEODR4 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEODR5 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEOv20100513 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
videoVarFrameSetInfo |
VIDEOv20111208 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vikingVarFrameSetInfo |
VIKINGv20110714 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCDR1 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCDR2 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCDR3 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCDR4 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCDR5 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20110816 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20110909 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20120126 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
|
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20121128 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20130304 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20130805 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20140428 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20140903 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20150309 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20151218 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20160311 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20160822 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20170109 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20170411 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20171101 |
Strateva parameter, c, in fit to photometric rms vs magnitude in Y band, see Sesar et al. 2007. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20180702 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20181120 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20191212 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20210708 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vmcVarFrameSetInfo |
VMCv20230816 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
ycStratPht |
vvvVarFrameSetInfo |
VVVDR5 |
Parameter, c2 from Ferreira-Lopes & Cross 2017, Eq. 18, in fit to photometric rms vs magnitude in Y band. |
real |
4 |
|
-0.9999995e9 |
stat.fit.param;em.IR.NIR |
The best fit solution to the expected RMS brightness (in magnitudes) for all objects in the frameset. Objects were binned in ranges of magnitude and the median RMS (after clipping out variable objects using the median-absolute deviation) was calculated. The Strateva function $\zeta(m)>=a+b\,10^{0.4m}+c\,10^{0.8m}$ was fit, where $\zeta(m)$ is the expected RMS as a function of magnitude. The chi-squared and number of degrees of freedom are also calculated. This technique was used in Sesar et al. 2007, AJ, 134, 2236. |
yDeblend |
vhsSourceRemeasurement |
VHSDR1 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
videoSource, videoSourceRemeasurement |
VIDEOv20100513 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vikingSourceRemeasurement |
VIKINGv20110714 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vikingSourceRemeasurement |
VIKINGv20111019 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vmcSourceRemeasurement |
VMCv20110816 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vmcSourceRemeasurement |
VMCv20110909 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vvvSource |
VVVv20110718 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
yDeblend |
vvvSource, vvvSourceRemeasurement |
VVVv20100531 |
placeholder flag indicating parent/child relation in Y |
int |
4 |
|
-99999999 |
meta.code |
ydec |
StackObjectThin |
PS1DR2 |
Declination from y filter stack detection. |
float |
8 |
degrees |
-999 |
|
ydecErr |
StackObjectThin |
PS1DR2 |
Declination error from y filter stack detection. |
real |
4 |
arcsec |
-999 |
|
Yell |
vvvParallaxCatalogue, vvvProperMotionCatalogue |
VVVDR5 |
Ellipticity of the DR4 Y detection. {catalogue TType keyword: Yell} |
real |
4 |
|
-999999500.0 |
|
yEll |
ultravistaSource |
ULTRAVISTADR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticty |
yEll |
vhsSource |
VHSDR2 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vhsSource |
VHSDR3 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSDR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSDR5 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSDR6 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20120926 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vhsSource |
VHSv20130417 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vhsSource |
VHSv20140409 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20150108 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20160114 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20160507 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20170630 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20180419 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource |
VHSv20201209 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vhsSource, vhsSourceRemeasurement |
VHSDR1 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
videoSource |
VIDEODR2 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
videoSource |
VIDEODR3 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
videoSource |
VIDEODR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
videoSource |
VIDEODR5 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
videoSource |
VIDEOv20111208 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
videoSource, videoSourceRemeasurement |
VIDEOv20100513 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGDR2 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGDR3 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGDR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource |
VIKINGv20111019 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGv20130417 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGv20140402 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingSource |
VIKINGv20150421 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource |
VIKINGv20151230 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource |
VIKINGv20160406 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource |
VIKINGv20161202 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource |
VIKINGv20170715 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vikingSource, vikingSourceRemeasurement |
VIKINGv20110714 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCDR2 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCDR3 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCDR4 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCDR5 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20110909 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCv20120126 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCv20121128 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCv20130304 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCv20130805 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource |
VMCv20140428 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20140903 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20150309 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20151218 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20160311 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20160822 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20170109 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20170411 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20171101 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20180702 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20181120 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20191212 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20210708 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource |
VMCv20230816 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vmcSource, vmcSourceRemeasurement |
VMCv20110816 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vmcSource, vmcSynopticSource |
VMCDR1 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vvvSource |
VVVDR2 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vvvSource |
VVVDR5 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity;em.IR.NIR |
yEll |
vvvSource |
VVVv20110718 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vvvSource, vvvSourceRemeasurement |
VVVv20100531 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yEll |
vvvSource, vvvSynopticSource |
VVVDR1 |
1-b/a, where a/b=semi-major/minor axes in Y |
real |
4 |
|
-0.9999995e9 |
src.ellipticity |
yeNum |
ultravistaMergeLog, ultravistaRemeasMergeLog |
ULTRAVISTADR4 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSDR1 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vhsMergeLog |
VHSDR2 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vhsMergeLog |
VHSDR3 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSDR4 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSDR5 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSDR6 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20120926 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vhsMergeLog |
VHSv20130417 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vhsMergeLog |
VHSv20140409 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20150108 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20160114 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20160507 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20170630 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20180419 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vhsMergeLog |
VHSv20201209 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.id;em.IR.NIR |
yeNum |
videoMergeLog |
VIDEODR2 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
videoMergeLog |
VIDEODR3 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
videoMergeLog |
VIDEODR4 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
videoMergeLog |
VIDEODR5 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
videoMergeLog |
VIDEOv20100513 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
videoMergeLog |
VIDEOv20111208 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGDR2 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGDR3 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGDR4 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingMergeLog |
VIKINGv20110714 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGv20111019 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGv20130417 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGv20140402 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingMergeLog |
VIKINGv20150421 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingMergeLog |
VIKINGv20151230 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingMergeLog |
VIKINGv20160406 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingMergeLog |
VIKINGv20161202 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingMergeLog |
VIKINGv20170715 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vikingZY_selJ_RemeasMergeLog |
VIKINGZYSELJv20160909 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vikingZY_selJ_RemeasMergeLog |
VIKINGZYSELJv20170124 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCDR2 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCDR3 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCDR4 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCDR5 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.id;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20110816 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20110909 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20120126 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20121128 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20130304 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20130805 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vmcMergeLog |
VMCv20140428 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20140903 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20150309 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20151218 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20160311 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20160822 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20170109 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20170411 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20171101 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20180702 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20181120 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20191212 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.id;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20210708 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.id;em.IR.NIR |
yeNum |
vmcMergeLog |
VMCv20230816 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.id;em.IR.NIR |
yeNum |
vmcMergeLog, vmcSynopticMergeLog |
VMCDR1 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vvvMergeLog |
VVVDR2 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vvvMergeLog |
VVVDR5 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number;em.IR.NIR |
yeNum |
vvvMergeLog |
VVVv20100531 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vvvMergeLog |
VVVv20110718 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yeNum |
vvvMergeLog, vvvSynopticMergeLog |
VVVDR1 |
the extension number of this Y frame |
tinyint |
1 |
|
|
meta.number |
yEpoch |
StackObjectThin |
PS1DR2 |
Modified Julian Date of the mean epoch of images contributing to the the y-band stack (equinox J2000). |
float |
8 |
days |
-999 |
|
Yerr |
decapsSource |
DECAPS |
Uncertainty in mean Y-band flux (statistical only) {catalogue TType keyword: err[5]} |
real |
4 |
3631Jy |
-9.999995e8 |
stat.error;phot.flux;em.IR.J |
yErr |
sharksDetection |
SHARKSv20210222 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
sharksDetection |
SHARKSv20210421 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
ultravistaDetection, ultravistaMapRemeasurement |
ULTRAVISTADR4 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSDR2 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSDR3 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSDR4 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSDR5 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSDR6 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20120926 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20130417 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20140409 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20150108 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20160114 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20160507 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20170630 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20180419 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection |
VHSv20201209 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vhsDetection, vhsListRemeasurement |
VHSDR1 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEODR2 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEODR3 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEODR4 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEODR5 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEOv20100513 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoDetection |
VIDEOv20111208 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
videoListRemeasurement |
VIDEOv20100513 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGDR2 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGDR3 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGDR4 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20111019 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20130417 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20140402 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20150421 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20151230 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20160406 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20161202 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection |
VIKINGv20170715 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingDetection, vikingListRemeasurement |
VIKINGv20110714 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingMapRemeasurement |
VIKINGZYSELJv20160909 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vikingMapRemeasurement |
VIKINGZYSELJv20170124 |
Error in Y coordinate (SE: ERRY2_IMAGE½) {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCDR1 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCDR2 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCDR3 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCDR4 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCDR5 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20110909 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20120126 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20121128 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20130304 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20130805 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20140428 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20140903 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20150309 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20151218 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20160311 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20160822 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20170109 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20170411 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20171101 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20180702 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20181120 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20191212 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20210708 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection |
VMCv20230816 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcDetection, vmcListRemeasurement |
VMCv20110816 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vmcdeepDetection |
VMCDEEPv20230713 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vvvDetection |
VVVDR1 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vvvDetection |
VVVDR2 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vvvDetection, vvvDetectionPawPrints, vvvDetectionTiles |
VVVDR5 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
yErr |
vvvDetection, vvvListRemeasurement |
VVVv20100531 |
Error in Y coordinate {catalogue TType keyword: Y_coordinate_err} Estimate of centroid error. |
real |
4 |
pixels |
|
stat.error |
Yerr_lbs |
decapsSource |
DECAPS |
Uncertainty in mean local background subtracted Y-band flux (statistical only) {catalogue TType keyword: err_lbs[5]} |
real |
4 |
3631Jy |
-9.999995e8 |
stat.error;phot.flux;em.IR.J |
YERR_R |
spectra |
SIXDF |
error on Y_R position |
int |
4 |
|
|
|
YERR_V |
spectra |
SIXDF |
error on Y_V position |
int |
4 |
|
|
|
yErrBits |
ultravistaSource |
ULTRAVISTADR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
ultravistaSourceRemeasurement |
ULTRAVISTADR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR1 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR2 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR3 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR5 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSDR6 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20120926 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20130417 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20140409 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20150108 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20160114 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20160507 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20170630 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20180419 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSource |
VHSv20201209 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vhsSourceRemeasurement |
VHSDR1 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
videoSource |
VIDEODR2 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSource |
VIDEODR3 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSource |
VIDEODR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSource |
VIDEODR5 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSource |
VIDEOv20100513 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSource |
VIDEOv20111208 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
This uses the FLAGS attribute in SE. The individual bit flags that this can be decomposed into are as follows: Bit Flag | Meaning | | 1 | The object has neighbours, bright enough and close enough to significantly bias the MAG_AUTO photometry or bad pixels (more than 10% of photometry affected). | | 2 | The object was originally blended with another | | 4 | At least one pixel is saturated (or very close to) | | 8 | The object is truncated (too close to an image boundary) | | 16 | Object's aperture data are incomplete or corrupted | | 32 | Object's isophotal data are imcomplete or corrupted. This is an old flag inherited from SE v1.0, and is kept for compatability reasons. It doesn't have any consequence for the extracted parameters. | | 64 | Memory overflow occurred during deblending | | 128 | Memory overflow occurred during extraction | |
|
yErrBits |
videoSourceRemeasurement |
VIDEOv20100513 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vikingSource |
VIKINGDR2 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGDR3 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGDR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20110714 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20111019 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20130417 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20140402 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20150421 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20151230 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20160406 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20161202 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSource |
VIKINGv20170715 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingSourceRemeasurement |
VIKINGv20110714 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vikingSourceRemeasurement |
VIKINGv20111019 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20160909 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vikingZY_selJ_SourceRemeasurement |
VIKINGZYSELJv20170124 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCDR2 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCDR3 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCDR4 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCDR5 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20110816 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20110909 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20120126 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20121128 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20130304 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20130805 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20140428 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20140903 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20150309 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20151218 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20160311 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20160822 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20170109 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20170411 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20171101 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20180702 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20181120 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20191212 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20210708 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource |
VMCv20230816 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSource, vmcSynopticSource |
VMCDR1 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vmcSourceRemeasurement |
VMCv20110816 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vmcSourceRemeasurement |
VMCv20110909 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vvvSource |
VVVDR2 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vvvSource |
VVVDR5 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code;em.IR.NIR |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vvvSource |
VVVv20100531 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vvvSource |
VVVv20110718 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vvvSource, vvvSynopticSource |
VVVDR1 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
Apparently not actually an error bit flag, but a count of the number of zero confidence pixels in the default (2 arcsec diameter) aperture. |
yErrBits |
vvvSourceRemeasurement |
VVVv20100531 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yErrBits |
vvvSourceRemeasurement |
VVVv20110718 |
processing warning/error bitwise flags in Y |
int |
4 |
|
-99999999 |
meta.code |
yEta |
ultravistaSource |
ULTRAVISTADR4 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR1 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR2 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR3 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR4 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR5 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSDR6 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20120926 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20130417 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20140409 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20150108 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20160114 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20160507 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20170630 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20180419 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vhsSource |
VHSv20201209 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEODR2 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEODR3 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEODR4 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEODR5 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEOv20100513 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
videoSource |
VIDEOv20111208 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGDR2 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGDR3 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGDR4 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20110714 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20111019 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20130417 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20140402 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20150421 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20151230 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20160406 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20161202 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vikingSource |
VIKINGv20170715 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCDR2 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCDR3 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCDR4 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCDR5 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20110816 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20110909 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20120126 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20121128 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20130304 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20130805 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20140428 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20140903 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20150309 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20151218 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20160311 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20160822 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20170109 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20170411 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20171101 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20180702 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20181120 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20191212 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20210708 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource |
VMCv20230816 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff;em.IR.NIR |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available passbands. |
yEta |
vmcSource, vmcSynopticSource |
VMCDR1 |
Offset of Y detection from master position (+north/-south) |
real |
4 |
arcsec |
-0.9999995e9 |
pos.eq.dec;arith.diff |
When associating individual passband detections into merged sources, a generous (in terms of the positional uncertainties) pairing radius of 1.0 arcseconds is used. Such a large association criterion can of course lead to spurious pairings in the merged sources lists (although note that between passband pairs, handshake pairing is done: both passbands must agree that the candidate pair is their nearest neighbour for the pair to propagate through into the merged source table). In order to help filter spurious pairings out, and assuming that large positional offsets between the different passband detections are not expected (e.g. because of source motion, or larger than usual positional uncertainties) then the attributes Xi and Eta can be used to filter any pairings with suspiciously large offsets in one or more bands. For example, for a clean sample of QSOs from the VHS, you might wish to insist that the offsets in the selected sample are all below 0.5 arcsecond: simply add WHERE clauses into the SQL sample selection script to exclude all Xi and Eta values larger than the threshold you want. NB: the master position is the position of the detection in the shortest passband in the set, rather than the ra/dec of the source as stored in source attributes of the same name. The former is used in the pairing process, while the latter is generally the optimally weighted mean position from an astrometric solution or other combinatorial process of all individual detection positions across the available pas |