W |
Name | Schema Table | Database | Description | Type | Length | Unit | Default Value | Unified Content Descriptor |
w1ab_map |
catwise_2020, catwise_prelim |
WISE |
w1 artifact code value |
int |
4 |
|
|
|
w1ab_map_str |
catwise_2020, catwise_prelim |
WISE |
w1 artifact string |
varchar |
13 |
|
|
|
w1ba |
allwise_sc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W1. |
float |
8 |
arcsec |
|
|
w1ba |
wise_allskysc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W1. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w1ba |
wise_prelimsc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W1 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w1cc_map |
allwise_sc |
WISE |
Contamination and confusion map for this source in W1. This column contains the integer equivalent of the 9-bit binary number that specifies if the W1 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
int |
4 |
|
|
|
The elements of the binary array are: S 0 0 0 O H 0 P D. The leftmost bit, S, differentiates whether the band-detection is believed to be a real detection contaminated by an artifact ("0") or a spurious detection of an artifact ("1"). The remaining bits are set to "1" to denote contamination by different types of artifacts according to the letters: - D - Diffraction spike. Source may be a spurious detection of or contaminated by a diffraction spike of a nearby bright star on the same image.
- P - Persistence. Source may be a spurious detection of or contaminated by a short-term latent (persistence) image left by a bright source.
- H - Halo. Source may be a spurious detection of or contaminated by the scattered light halo associated with a bright star.
- O (letter "o") - Optical ghost. Source may be a spurious detection of or contaminated by an optical ghost image caused by a nearby bright source on the same image.
For example, a measurement that is believed to be a spurious detection of a diffraction spike and scattered light halo has a binary bit map value of "100001001" and w?cc_map=265. |
w1cc_map |
catwise_2020, catwise_prelim |
WISE |
worst case w1cc_map from AllWISE |
int |
4 |
|
|
|
w1cc_map |
wise_allskysc |
WISE |
Contamination and confusion map for this source in W1. This column contains the integer equivalent of the 9-bit binary number that specifies if the W1 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
smallint |
2 |
|
|
|
w1cc_map |
wise_prelimsc |
WISE |
Contamination and confusion map for this source in W1 This column contains the integer equivalent of the 9-bit binary number that specifies if the W1 measurement is believed to be contaminated by or a spurious detection of an image artifact |
smallint |
2 |
|
|
|
w1cc_map_str |
allwise_sc |
WISE |
Contamination and confusion string. This column is a character string that denotes all artifacts that may contaminate the W1 measurement of this source, in the priority order D,P,H,O,d,p,h,o. Lower-case letters denote cases where the source detection in this band is believed to be real but the measurement may be contaminated by the artifact. upper-case letters denote cases where the source detection in this band may be a spurious detection of an artifact. This string is "null" if there are no artifacts that affect the measurement in this band. The value that appears in first element of the cc_flags string is the left-most character in w1cc_map_str. If w1cc_map_str is "null", then the corresponding cc_flags entry is "0". |
varchar |
9 |
|
|
|
For example, a real detection that is contaminated by a diffraction spike and a latent (persistent) image has a w?cc_map_str="dp". A spurious detection of a diffraction spike that is also contaminated by a latent image has w?cc_map_str="Dp". |
w1cc_map_str |
catwise_2020, catwise_prelim |
WISE |
worst case w1cc_map_str from AllWISE |
varchar |
20 |
|
|
|
w1cc_map_str |
wise_allskysc |
WISE |
Contamination and confusion string in W1. This column is a character string that denotes all artifacts that may contaminate the W1 measurement of this source, in the priority order D,P,H,O,d,p,h,o. |
char |
9 |
|
|
|
w1cc_map_str |
wise_prelimsc |
WISE |
Contamination and confusion string in W1 This column is a character string that denotes all artifacts that may contaminate the W1 measurement of this source, in the priority order D,P,H,O |
char |
9 |
|
|
|
w1conf |
allwise_sc |
WISE |
Estimated confusion noise in the W1 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w1sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
dn |
|
|
w1conf |
catwise_2020, catwise_prelim |
WISE |
frame sky confusion based on the UNC images |
real |
4 |
dn |
|
|
w1conf |
wise_allskysc |
WISE |
Estimated confusion noise in the W1 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w1sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
ADU |
-0.9999995e9 |
|
w1conf |
wise_prelimsc |
WISE |
Estimated confusion noise in the W1 sky background annulus, in digital numbers This number is the difference between the measured noise in the sky background w1sigsk and the noise measured in the same region on the Atlas Uncertainty Maps |
float |
8 |
ADU |
-0.9999995e9 |
|
w1Cov |
catwise_2020, catwise_prelim |
WISE |
mean coverage depth, band-1 |
real |
4 |
|
|
|
w1cov |
allwise_sc |
WISE |
Mean pixel coverage in W1. This column gives the mean pixel value from the W1 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
float |
8 |
|
|
|
W1cov may differ from the integer frame coverage value given in w1m for two reasons. First, individual pixels in the measurement area may be masked or otherwise unusable, reducing the effective pixel count and thus the mean coverage value. Second, the effective sky area sampled by a pixels in single-exposure image varies across the focal plane because of field distortion. Distortion is corrected when coadding to generate the Atlas Images. Therefore, the effective number of pixels contributing to a pixel in the Atlas Coverage Map may be slightly smaller or larger than expected if there was no distortion. Third, the values of w1m may be artificially reduced for sources that are covered by saturated 3-Band Cryo single-exposures. |
w1cov |
wise_allskysc |
WISE |
Mean pixel coverage in W1. This column gives the mean pixel value from the W1 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
real |
4 |
|
-0.9999995e9 |
|
w1cov |
wise_prelimsc |
WISE |
Mean pixel coverage in W1 This column gives the mean pixel value from the W1 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
real |
4 |
|
-0.9999995e9 |
|
w1dmag |
wise_allskysc |
WISE |
Difference between maximum and minimum magnitude of the source from all usable single-exposure frames, W1. Single-exposure measurements with w1rchi2 values greater than 3.0 times the median are rejected from this computation. |
real |
4 |
mag |
-0.9999995e9 |
|
w1fitr |
catwise_2020, catwise_prelim |
WISE |
fitting radius, band-1 (clipped at 999.99) |
real |
4 |
asec |
|
|
w1flg |
allwise_sc |
WISE |
W1 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg |
catwise_2020, catwise_prelim |
WISE |
standard aperture flag, band-1 |
int |
4 |
|
|
|
Standard aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise ususable pixels, or is an upper limit. The flag value is the integer sum of any of following values which correspond to different conditions: - 0 - nominal: no contamination
- 1 - source confusion: another source falls within the measurement aperture/li>
- 2 - bad or fatal pixels: presence of bad pixels in the measurement aperture (bit 2 or 18 set)
- 4 - non-zero bit flag tripped (other than 2 or 18)
- 8 - corruption: all pixels are flagged as unusable, or the aperture flux is negative; in the former case, the aperture magnitude is "null"; in the latter case, the aperture magnitude is a 95% confidence upper limit
- 16 - saturation: here are one or more saturated pixels in the measurement aperture
- 32 - upper limit: the magnitude is a 95% confidence upper limit
Note about upper limits: threshold = 2 * RMS if ( f < threshold) then if (f < 0) then upper_limit = threshold else upper_limit = f + threshold where f is the flux of the source, RMS is the source flux uncertainty. The upper limit is reported in the WPRO and standard aperture MAG columns; the reported uncertainty is set to 9.99 mag. |
w1flg |
wise_allskysc |
WISE |
W1 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
smallint |
2 |
|
-9999 |
|
w1flg |
wise_prelimsc |
WISE |
W1 "standard" aperture measurement quality flag This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit |
smallint |
2 |
|
-9999 |
|
w1flg_1 |
allwise_sc |
WISE |
W1 5.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_1 |
wise_allskysc |
WISE |
W1 5.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_1 |
wise_prelimsc |
WISE |
W1 5.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_2 |
allwise_sc |
WISE |
W1 8.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_2 |
wise_allskysc |
WISE |
W1 8.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_2 |
wise_prelimsc |
WISE |
W1 8.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_3 |
allwise_sc |
WISE |
W1 11.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_3 |
wise_allskysc |
WISE |
W1 11.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_3 |
wise_prelimsc |
WISE |
W1 11.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_4 |
allwise_sc |
WISE |
W1 13.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_4 |
wise_allskysc |
WISE |
W1 13.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_4 |
wise_prelimsc |
WISE |
W1 13.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_5 |
allwise_sc |
WISE |
W1 16.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_5 |
wise_allskysc |
WISE |
W1 16.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_5 |
wise_prelimsc |
WISE |
W1 16.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_6 |
allwise_sc |
WISE |
W1 19.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_6 |
wise_allskysc |
WISE |
W1 19.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_6 |
wise_prelimsc |
WISE |
W1 19.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_7 |
allwise_sc |
WISE |
W1 22.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_7 |
wise_allskysc |
WISE |
W1 22.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_7 |
wise_prelimsc |
WISE |
W1 22.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flg_8 |
allwise_sc |
WISE |
W1 24.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1flg_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture flag, band-1 |
int |
4 |
|
|
|
w1flg_8 |
wise_allskysc |
WISE |
W1 24.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w1flg_8 |
wise_prelimsc |
WISE |
W1 24.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1flux |
allwise_sc |
WISE |
The "raw" W1 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w1flux |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux, band-1 |
real |
4 |
dn |
|
|
w1flux |
wise_allskysc |
WISE |
The "raw" W1 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w1flux |
wise_prelimsc |
WISE |
The "raw" W1 source flux measured in profile-fit photometry in units of digital numbers This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w1flux_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux, band-1 |
real |
4 |
dn |
|
|
w1frl |
wise_prelimsc |
WISE |
Fraction of W1 pixels affected by latents This column gives the fraction of all W1 pixels in the stack of individual W1 exposures used to characterize this source that may be affected by the presence of a latent image produced by a bright source |
real |
4 |
|
-0.9999995e9 |
|
w1frtr |
wise_allskysc |
WISE |
Fraction of W1 pixels affected by transients. This column gives the fraction of all W1 pixels in the stack of individual W1 exposures used to characterize this source that may be affected by transient events. This number is computed by counting the number of pixels in the single exposure Bit Mask images with value "21" that are present within the profile-fitting area, a circular region with radius of 7.25", centered on the position of this source, and dividing by the total number of pixels in the same area that are available for measurement. |
real |
4 |
|
-0.9999995e9 |
|
w1gerr |
allwise_sc |
WISE |
Uncertainty in the W1 magnitude of source measured in elliptical aperture. CAUTION: A w1gerr value of 9.999 indicates that the measurement uncertainty is very large, or the uncertainty could not be computed. In either case, the w1gmag measurement should be considered highly suspect. |
float |
8 |
mag |
|
|
w1gerr |
wise_allskysc |
WISE |
Uncertainty in the W1 magnitude of source measured in elliptical aperture. |
real |
4 |
mag |
-0.9999995e9 |
|
w1gerr |
wise_prelimsc |
WISE |
Uncertainty in the W1 magnitude of source measured in elliptical aperture |
real |
4 |
mag |
-0.9999995e9 |
|
w1gflg |
allwise_sc |
WISE |
W1 elliptical aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w1gflg |
wise_allskysc |
WISE |
W1 elliptical aperture measurement quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag, w1mflg. |
smallint |
2 |
|
-9999 |
|
w1gflg |
wise_prelimsc |
WISE |
W1 elliptical aperture measurement quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w1gmag |
allwise_sc |
WISE |
W1 magnitude of source measured in the elliptical aperture described by w1rsemi, w1ba, and w1pa. |
float |
8 |
mag |
|
|
w1gmag |
wise_allskysc |
WISE |
W1 magnitude of source measured in the elliptical aperture described by w1rsemi, w1ba, and w1pa. |
real |
4 |
mag |
-0.9999995e9 |
|
w1gmag |
wise_prelimsc |
WISE |
W1 magnitude of source measured in the elliptical aperture described by w1rsemi, w1ba, and w1pa |
real |
4 |
mag |
-0.9999995e9 |
|
w1k |
allwise_sc |
WISE |
Stetson K variability index (Stetson, P. 1996, PASP, 108, 851) computed using the W1 profile-fit fluxes measured on the individual single-exposure images. This column is null if there are <3 single-exposure measurements available in W1. |
float |
8 |
|
|
|
w1k |
catwise_2020, catwise_prelim |
WISE |
Stetson k index for variability; band-1 |
real |
4 |
|
|
|
w1M |
catwise_2020, catwise_prelim |
WISE |
WPRO, M , band-1 M == number of flux measurements for a given source |
int |
4 |
|
|
|
w1m |
allwise_sc |
WISE |
Integer frame coverage. This column gives the number of individual 7.7s W1 exposures on which a profile-fit measurement of this source was possible. This number can differ between the four bands because band-dependent criteria are used to select individual frames for inclusion in the coadded Atlas Images. This column is null if there is no frame coverage in this band at the position of this source. CAUTION: The value of w1m may be lower than expected for sources that were covered by saturated 3-Band Cryo single-exposures. A sign of this is if w1m differs significantly from w1cov. |
int |
4 |
|
|
|
w1m |
wise_allskysc |
WISE |
Integer frame coverage in W1. This column gives the number of individual 7.7s W1 exposures on which a profile-fit measurement of this source was possible. |
bigint |
8 |
|
-99999999 |
|
w1m |
wise_prelimsc |
WISE |
Integer frame coverage in W1 This column gives the number of individual 7.7s W1 exposures on which a profile-fit measurement of this source was possible |
bigint |
8 |
|
-99999999 |
|
w1mag |
allwise_sc |
WISE |
W1 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". The curve-of-growth correction is given in w1mcor. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag |
catwise_2020, catwise_prelim |
WISE |
standard aperture mag w/ correction applied |
real |
4 |
mag |
|
|
w1mag |
wise_allskysc |
WISE |
W1 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag |
wise_prelimsc |
WISE |
W1 "standard" aperture magnitude This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_1 |
allwise_sc |
WISE |
W1 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
|
|
|
w1mag_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_1 |
wise_allskysc |
WISE |
W1 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_1 |
wise_prelimsc |
WISE |
W1 5.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_2 |
allwise_sc |
WISE |
W1 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_2 |
wise_allskysc |
WISE |
W1 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_2 |
wise_prelimsc |
WISE |
W1 8.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_3 |
allwise_sc |
WISE |
W1 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_3 |
wise_allskysc |
WISE |
W1 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_3 |
wise_prelimsc |
WISE |
W1 11.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_4 |
allwise_sc |
WISE |
W1 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_4 |
wise_allskysc |
WISE |
W1 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_4 |
wise_prelimsc |
WISE |
W1 13.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_5 |
allwise_sc |
WISE |
W1 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_5 |
wise_allskysc |
WISE |
W1 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_5 |
wise_prelimsc |
WISE |
W1 16.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_6 |
allwise_sc |
WISE |
W1 19.25" radius aperture magnitude. This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_6 |
wise_allskysc |
WISE |
W1 19.25" radius aperture magnitude. This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_6 |
wise_prelimsc |
WISE |
W1 19.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_7 |
allwise_sc |
WISE |
W1 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_7 |
wise_allskysc |
WISE |
W1 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_7 |
wise_prelimsc |
WISE |
W1 22.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_8 |
allwise_sc |
WISE |
W1 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W1. |
float |
8 |
mag |
|
|
w1mag_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture mag, band-1 |
real |
4 |
mag |
|
|
w1mag_8 |
wise_allskysc |
WISE |
W1 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W1. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mag_8 |
wise_prelimsc |
WISE |
W1 24.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W1 |
real |
4 |
mag |
-0.9999995e9 |
|
W1mag_ALLWISE |
ravedr5Source |
RAVE |
W1 magnitude from ALLWISE |
real |
4 |
mag |
|
phot.mag;em.opt |
w1magP |
catwise_2020, catwise_prelim |
WISE |
WPRO repeatability mag; band-1 |
real |
4 |
mag |
|
|
w1magp |
allwise_sc |
WISE |
Magnitude computed from the inverse-variance-weighted mean of the profile-fit flux measurements on the w1m individual W1 frames covering this source. This differs from w1mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w1mpro is computed by fitting all W1 frames simultaneously and incorporating a robust error model. This column is "null" if w1m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w1mpro for the optimal flux measurement for point sources. |
float |
8 |
mag |
|
|
w1magp |
wise_allskysc |
WISE |
Inverse-variance-weighted mean W1 magnitude computed from profile-fit measurements on the w1m individual frames covering this source. This differs from w1mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w1mpro is computed by fitting all W1 frames simultaneously and incorporating a robust error model. This column is default if w1m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w1mpro for the optimal flux measurement for point sources. |
real |
4 |
mag |
-0.9999995e9 |
|
w1magp |
wise_prelimsc |
WISE |
Inverse-variance-weighted mean W1 magnitude computed from profile-fit measurements on the w1m individual frames covering this source This differs from w1mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w1mpro is computed by fitting all W1 frames simultaneously and incorporating a robust error model. This column is default if w1m=0, the mean flux is negative or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mcor |
allwise_sc |
WISE |
W1 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w1mag_2, to give the "standard-aperture" magnitude. |
float |
8 |
mag |
|
|
w1mcor |
wise_allskysc |
WISE |
W1 aperture curve-of-growth correction. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w1mag_2, to give the "standard-aperture" magnitude. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mcor |
wise_prelimsc |
WISE |
W1 aperture curve-of-growth correction This correction is subtracted from the nominal 8.25" aperture photometry brightness, w1mag_2, to give the "standard-aperture" magnitude |
real |
4 |
mag |
-0.9999995e9 |
|
w1mCorr |
twompzPhotoz |
TWOMPZ |
WISE w1mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: W1mCorr} |
real |
4 |
|
-0.9999995e9 |
|
w1mCorr |
wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm |
WISExSCOSPZ |
WISE w1mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: W1C} |
real |
4 |
|
-0.9999995e9 |
|
w1mCorrErr |
twompzPhotoz |
TWOMPZ |
W1 profile fit photometric measurement uncertainty {image primary HDU keyword: w1sigmpro} |
real |
4 |
mag |
-0.9999995e9 |
|
w1mCorrErr |
wiseScosSvm |
WISExSCOSPZ |
Error on WISE w1mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: w1sigmpro} |
real |
4 |
|
-0.9999995e9 |
|
w1mJDmax |
catwise_2020, catwise_prelim |
WISE |
maximum mJD; band-1 |
float |
8 |
|
|
|
w1mjdmax |
allwise_sc, wise_allskysc |
WISE |
The latest modified Julian Date (mJD) of the W1 single-exposures covering the source. |
float |
8 |
|
|
|
w1mJDmea |
catwise_2020, catwise_prelim |
WISE |
mean mJD; band-1 |
float |
8 |
|
|
|
w1mjdmean |
allwise_sc, wise_allskysc |
WISE |
The average modified Julian Date (mJD) of the W1 single-exposures covering the source. |
float |
8 |
|
|
|
w1mJDmin |
catwise_2020, catwise_prelim |
WISE |
minimum mJD; band-1 |
float |
8 |
|
|
|
w1mjdmin |
allwise_sc, wise_allskysc |
WISE |
The earliest modified Julian Date (mJD) of the W1 single-exposures covering the source. |
float |
8 |
|
|
|
w1mLQ |
catwise_2020, catwise_prelim |
WISE |
-log(Q), Q = 1-P(chi-square); band-1 |
real |
4 |
|
|
|
w1mlq |
allwise_sc |
WISE |
Probability measure that the source is variable in W1 flux. The value is -ln(Q), where Q = 1 - P(χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
float |
8 |
|
|
|
The Q value is the fraction of all cases to be at least as large as that observed if the null hypothesis is true. The null hypothesis is that the flux is emitted by a non-variable astrophysical object. It may be false because the object is a true variable. It may also be false because the flux measurement is corrupted by artifacts such as cosmic rays, scattered light, etc. The smaller the Q value, the more implausible the null hypothesis, i.e., the more likely it is that the flux is either variable or corrupted or both. |
w1mlq |
wise_allskysc |
WISE |
Probability measure that the source is variable in W1 flux. The value is -log10(Q), where Q = 1 - P(Χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
int |
4 |
|
-99999999 |
|
w1mpro |
allwise_sc |
WISE |
W1 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W1 flux measurement has SNR<2. This column is null if the source is nominally detected in W1, but no useful brightness estimate could be made. |
float |
8 |
mag |
|
|
NOTE: A special exception to the upper limit conditions described above applies if the W1 value of ph_qual is "Z" (e.g. ph_qual LIKE 'Z%'). In these cases, the value of w1mpro corresponds to the actual flux measurement, w1flux, or is null if w1flux is negative. This occurs for 106,140 sources in the AllWISE Catalog and 54,900 sources in the Reject Table, all of which are confined to a narrow strip of ecliptic longitude. |
w1mpro |
catwise_2020, catwise_prelim |
WISE |
WPRO flux in mag units, band-1 |
real |
4 |
mag |
|
|
w1mpro |
wise_allskysc |
WISE |
W1 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W1 flux measurement has SNR<2. This column is default if the source is nominally detected in W1, but no useful brightness estimate could be made. |
real |
4 |
mag |
-0.9999995e9 |
|
w1mpro |
wise_prelimsc |
WISE |
W1 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W1 flux measurement has SNR<2 This column is default if the source is nominally detected in W1, but no useful brightness estimate could be made |
real |
4 |
mag |
-0.9999995e9 |
|
w1mpro_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO flux in mag units, band-1 |
real |
4 |
mag |
|
|
w1Ndf |
catwise_2020, catwise_prelim |
WISE |
No. degrees of freedom in var chi-square; band-1 |
int |
4 |
|
|
|
w1ndf |
allwise_sc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W1. |
int |
4 |
|
|
|
w1ndf |
wise_allskysc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W1. |
bigint |
8 |
|
-99999999 |
|
w1NM |
catwise_2020, catwise_prelim |
WISE |
WPRO, N (of M), band-1 M == number of flux measurements for a given source; N == number of M sources that have SNR >= 3 |
int |
4 |
|
|
|
w1nm |
allwise_sc |
WISE |
Integer frame detection count. This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W1 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
int |
4 |
|
|
|
w1nm |
wise_allskysc |
WISE |
Integer frame detection count in W1. This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W1 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
bigint |
8 |
|
-99999999 |
|
w1nm |
wise_prelimsc |
WISE |
Integer frame detection count in W1 This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W1 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures |
bigint |
8 |
|
-99999999 |
|
w1pa |
allwise_sc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W1. |
float |
8 |
deg |
|
|
w1pa |
wise_allskysc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W1. |
real |
4 |
degrees |
-0.9999995e9 |
|
w1pa |
wise_prelimsc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W1 |
real |
4 |
degrees |
-0.9999995e9 |
|
w1rchi2 |
allwise_sc |
WISE |
Reduced χ2 of the W1 profile-fit photometry measurement. This column is null if the W1 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
|
|
w1rchi2 |
catwise_2020, catwise_prelim |
WISE |
WPRO reduced chi^2, band-1 |
real |
4 |
|
|
|
w1rchi2 |
wise_allskysc |
WISE |
Reduced chi-squared of the W1 profile-fit photometry measurement. This column is default if the W1 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
-0.9999995e9 |
|
w1rchi2 |
wise_prelimsc |
WISE |
Reduced chi-squared of the W1 profile-fit photometry measurement This column is default if the W1 magnitude is a 95% confidence upper limit (i.e. the source is not detected) |
real |
4 |
|
-0.9999995e9 |
|
w1rchi2_pm |
allwise_sc |
WISE |
Reduced χ2 of the W1 profile-fit photometry measurement including motion estimation. This column is null if the source is not detected in W1, or if the motion fit failed to converge or was not attempted. |
real |
4 |
|
|
|
w1rchi2_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO reduced chi^2, band-1 |
real |
4 |
|
|
|
w1rsemi |
allwise_sc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W1. |
float |
8 |
arcsec |
|
|
w1rsemi |
wise_allskysc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W1. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w1rsemi |
wise_prelimsc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W1 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w1Sat |
catwise_2020, catwise_prelim |
WISE |
fraction of pixels saturated, band-1 |
real |
4 |
|
|
|
w1sat |
allwise_sc |
WISE |
Saturated pixel fraction, W1. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W1]~8 mag. Saturation may occur in fainter sources because of charged particle strikes, or if the source is covered by 3-Band Cryo single-exposures that began to saturate because of rising temperatures. |
float |
8 |
|
|
|
w1sat |
wise_allskysc |
WISE |
Saturated pixel fraction, W1. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W1]∼8 mag. Saturation may occur in fainter sources because of a charged particle strike. |
real |
4 |
|
-0.9999995e9 |
|
w1sat |
wise_prelimsc |
WISE |
Saturated pixel fraction, W1 The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation |
real |
4 |
|
-0.9999995e9 |
|
w1sigflux |
allwise_sc |
WISE |
Uncertainty in the "raw" W1 source flux measurement in profile-fit photometry in units of digital numbers. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w1sigflux |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux uncertainty, band-1 |
real |
4 |
dn |
|
|
w1sigflux |
wise_allskysc |
WISE |
Uncertainty in the "raw" W1 source flux measurement in profile-fit photometry in units of digital numbers This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w1sigflux |
wise_prelimsc |
WISE |
Uncertainty in the "raw" W1 source flux measurement in profile-fit photometry in units of digital numbers This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w1sigflux_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux uncertainty, band-1 |
real |
4 |
dn |
|
|
w1sigm |
allwise_sc |
WISE |
Uncertainty in the W1 "standard" aperture magnitude. This column is null if the W1 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm |
catwise_2020, catwise_prelim |
WISE |
standard aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm |
wise_allskysc |
WISE |
Uncertainty in the W1 "standard" aperture magnitude. This column is default if the W1 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm |
wise_prelimsc |
WISE |
Uncertainty in the W1 "standard" aperture magnitude This column is default if the W1 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_1 |
allwise_sc |
WISE |
Uncertainty in the W1 5.5" radius aperture magnitude. This column is null if the the 5.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_1 |
wise_allskysc |
WISE |
Uncertainty in the W1 5.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_1 |
wise_prelimsc |
WISE |
Uncertainty in the W1 5.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_2 |
allwise_sc |
WISE |
Uncertainty in the W1 8.25" radius aperture magnitude. This column is null if the the 8.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_2 |
wise_allskysc |
WISE |
Uncertainty in the W1 8.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_2 |
wise_prelimsc |
WISE |
Uncertainty in the W1 8.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_3 |
allwise_sc |
WISE |
Uncertainty in the W1 11.0" radius aperture magnitude. This column is null if the the 11.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_3 |
wise_allskysc |
WISE |
Uncertainty in the W1 11.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_3 |
wise_prelimsc |
WISE |
Uncertainty in the W1 11.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_4 |
allwise_sc |
WISE |
Uncertainty in the W1 13.75" radius aperture magnitude. This column is null if the the 13.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_4 |
wise_allskysc |
WISE |
Uncertainty in the W1 13.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_4 |
wise_prelimsc |
WISE |
Uncertainty in the W1 13.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_5 |
allwise_sc |
WISE |
Uncertainty in the W1 16.5" radius aperture magnitude. This column is null if the the 16.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_5 |
wise_allskysc |
WISE |
Uncertainty in the W1 16.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_5 |
wise_prelimsc |
WISE |
Uncertainty in the W1 16.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_6 |
allwise_sc |
WISE |
Uncertainty in the W1 19.25" radius aperture magnitude. This column is null if the the 19.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_6 |
wise_allskysc |
WISE |
Uncertainty in the W1 19.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_6 |
wise_prelimsc |
WISE |
Uncertainty in the W1 19.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_7 |
allwise_sc |
WISE |
Uncertainty in the W1 22.0" radius aperture magnitude. This column is null if the the 22.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_7 |
wise_allskysc |
WISE |
Uncertainty in the W1 22.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_7 |
wise_prelimsc |
WISE |
Uncertainty in the W1 22.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_8 |
allwise_sc |
WISE |
Uncertainty in the W1 24.75" radius aperture magnitude. This column is null if the the 24.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w1sigm_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture mag uncertainty, band-1 |
real |
4 |
mag |
|
|
w1sigm_8 |
wise_allskysc |
WISE |
Uncertainty in the W1 24.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigm_8 |
wise_prelimsc |
WISE |
Uncertainty in the W1 24.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigmpro |
allwise_sc |
WISE |
W1 profile-fit photometric measurement uncertainty in mag units. This column is null if the W1 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
float |
8 |
mag |
|
|
Note - In a small number of cases where the W1 value of ph_qual is "Z" (e.g. ph_qual LIKE 'Z%'), the W1 source flux uncertainty was not measurable because of the presence of a large number of saturated pixels from 3-Band Cryo frames covered the source. In these cases, this column is null, but the w1mpro column will correspond either to the actual source flux, w1flux, rather than the 95% confidence upper limit, or will be null if w1flux is negative. |
w1sigmpro |
catwise_2020, catwise_prelim |
WISE |
WPRO flux uncertainty in mag units, band-1 |
real |
4 |
mag |
|
|
w1sigmpro |
wise_allskysc |
WISE |
W1 profile-fit photometric measurement uncertainty. This column is default if the W1 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigmpro |
wise_prelimsc |
WISE |
W1 profile-fit photometric measurement uncertainty This column is default if the W1 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigmpro_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO flux uncertainty in mag units, band-1 |
real |
4 |
mag |
|
|
w1sigP1 |
catwise_2020, catwise_prelim |
WISE |
WPRO mag population sigma; band-1 |
real |
4 |
mag |
|
|
w1sigp1 |
allwise_sc |
WISE |
Standard deviation of the population of W1 fluxes measured on the w1m individual frames covering this source, in magnitudes. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is "null" if w1m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w1sigp1 |
wise_allskysc |
WISE |
Standard deviation of the population of W1 fluxes measured on the w1m individual frames covering this source. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w1m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigp1 |
wise_prelimsc |
WISE |
Standard deviation of the population of W1 fluxes measured on the w1m individual frames covering this source This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w1m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigP2 |
catwise_2020, catwise_prelim |
WISE |
WPRO mag uncertainty of the mean; band-1 |
real |
4 |
mag |
|
|
w1sigp2 |
allwise_sc |
WISE |
Standard deviation of the mean of the distribution of W1 fluxes (w1magp) computed from profile-fit measurements on the w1m individual frames covering this source, in magnitudes. This is equivalent to w1sigp1/sqrt(w1m). This column is "null" if w1m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w1sigp2 |
wise_allskysc |
WISE |
Standard deviation of the mean of the distribution of W1 fluxes (w1magp) computed from profile-fit measurements on the w1m individual frames covering this source. This column is default if w1m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigp2 |
wise_prelimsc |
WISE |
Standard deviation of the mean of the distribution of W1 fluxes (w1magp) computed from profile-fit measurements on the w1m individual frames covering this source This column is default if w1m<2 or if no individual frame measurements are possible |
real |
4 |
mag |
-0.9999995e9 |
|
w1sigsk |
allwise_sc |
WISE |
The uncertainty in the W1 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
float |
8 |
dn |
|
|
w1sigsk |
catwise_2020, catwise_prelim |
WISE |
frame sky background value uncertainty, band-1 |
real |
4 |
dn |
|
|
w1sigsk |
wise_allskysc |
WISE |
The uncertainty in the W1 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
real |
4 |
ADU |
-0.9999995e9 |
|
w1sigsk |
wise_prelimsc |
WISE |
The uncertainty in the W1 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" |
real |
4 |
ADU |
-0.9999995e9 |
|
w1sky |
allwise_sc |
WISE |
The trimmed average of the W1 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
dn |
|
|
For profile-fit photometry, the sky background is measured on the individual single-exposure images that are used for source characterization. For aperture photometry, the sky background is measured on the Atlas Image. |
w1sky |
catwise_2020, catwise_prelim |
WISE |
frame sky background value, band-1 |
real |
4 |
dn |
|
|
w1sky |
wise_allskysc |
WISE |
The trimmed average of the W1 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
ADU |
-0.9999995e9 |
|
w1sky |
wise_prelimsc |
WISE |
The trimmed average of the W1 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value |
float |
8 |
ADU |
-0.9999995e9 |
|
w1snr |
allwise_sc |
WISE |
W1 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w1flux) to flux uncertainty (w1sigflux)in the W1 profile-fit photometry measurement. This column is null if w1flux is negative, or if w1flux or w1sigflux are null. |
float |
8 |
|
|
|
w1snr |
catwise_2020, catwise_prelim |
WISE |
S/N ratio, band-1 |
real |
4 |
|
|
|
w1snr |
wise_allskysc |
WISE |
W1 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w1flux) to flux uncertainty (w1sigflux) in the W1 profile-fit photometry measurement. This column is default if w1flux is negative, or if w1flux or w1sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w1snr |
wise_prelimsc |
WISE |
W1 profile-fit measurement signal-to-noise ratio This value is the ratio of the flux (w1flux) to flux uncertainty (w1sigflux)in the W1 profile-fit photometry measurement. This column is default if w1flux is negative, or if w1flux or w1sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w1snr_pm |
catwise_2020, catwise_prelim |
WISE |
flux S/N ratio, band-1 |
real |
4 |
|
|
|
w2ab_map |
catwise_2020, catwise_prelim |
WISE |
w2 artifact code value |
int |
4 |
|
|
|
w2ab_map_str |
catwise_2020, catwise_prelim |
WISE |
w2 artifact string |
varchar |
13 |
|
|
|
w2ba |
allwise_sc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W2. |
float |
8 |
arcsec |
|
|
w2ba |
wise_allskysc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W2. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w2ba |
wise_prelimsc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W2 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w2cc_map |
allwise_sc |
WISE |
Contamination and confusion map for this source in W2. This column contains the integer equivalent of the 9-bit binary number that specifies if the W2 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
int |
4 |
|
|
|
The elements of the binary array are: S 0 0 0 O H 0 P D. The leftmost bit, S, differentiates whether the band-detection is believed to be a real detection contaminated by an artifact ("0") or a spurious detection of an artifact ("1"). The remaining bits are set to "1" to denote contamination by different types of artifacts according to the letters: - D - Diffraction spike. Source may be a spurious detection of or contaminated by a diffraction spike of a nearby bright star on the same image.
- P - Persistence. Source may be a spurious detection of or contaminated by a short-term latent (persistence) image left by a bright source.
- H - Halo. Source may be a spurious detection of or contaminated by the scattered light halo associated with a bright star.
- O (letter "o") - Optical ghost. Source may be a spurious detection of or contaminated by an optical ghost image caused by a nearby bright source on the same image.
For example, a measurement that is believed to be a spurious detection of a diffraction spike and scattered light halo has a binary bit map value of "100001001" and w?cc_map=265. |
w2cc_map |
catwise_2020, catwise_prelim |
WISE |
worst case w2cc_map from AllWISE |
int |
4 |
|
|
|
w2cc_map |
wise_allskysc |
WISE |
Contamination and confusion map for this source in W2. This column contains the integer equivalent of the 9-bit binary number that specifies if the W2 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
smallint |
2 |
|
|
|
w2cc_map |
wise_prelimsc |
WISE |
Contamination and confusion map for this source in W2 This column contains the integer equivalent of the 9-bit binary number that specifies if the W2 measurement is believed to be contaminated by or a spurious detection of an image artifact |
smallint |
2 |
|
|
|
w2cc_map_str |
allwise_sc |
WISE |
Contamination and confusion string. This column is a character string that denotes all artifacts that may contaminate the W2 measurement of this source, in the priority order D,P,H,O,d,p,h,o. Lower-case letters denote cases where the source detection in this band is believed to be real but the measurement may be contaminated by the artifact. Upper-case letters denote cases where the source detection in this band may be a spurious detection of an artifact. This string is "null" if there are no artifacts that affect the measurement in this band. The value that appears in second element of the cc_flags string is the left-most character in w2cc_map_str. If w2cc_map_str is "null", then the corresponding cc_flags entry is "0". |
varchar |
9 |
|
|
|
For example, a real detection that is contaminated by a diffraction spike and a latent (persistent) image has a w?cc_map_str="dp". A spurious detection of a diffraction spike that is also contaminated by a latent image has w?cc_map_str="Dp". |
w2cc_map_str |
catwise_2020, catwise_prelim |
WISE |
worst case w2cc_map_str from AllWISE |
varchar |
20 |
|
|
|
w2cc_map_str |
wise_allskysc |
WISE |
Contamination and confusion string in W2. This column is a character string that denotes all artifacts that may contaminate the W2 measurement of this source, in the priority order D,P,H,O,d,p,h,o. |
char |
9 |
|
|
|
w2cc_map_str |
wise_prelimsc |
WISE |
Contamination and confusion string in W2 This column is a character string that denotes all artifacts that may contaminate the W2 measurement of this source, in the priority order D,P,H,O |
char |
9 |
|
|
|
w2conf |
allwise_sc |
WISE |
Estimated confusion noise in the W2 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w2sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
dn |
|
|
w2conf |
catwise_2020, catwise_prelim |
WISE |
frame sky confusion based on the UNC images |
real |
4 |
dn |
|
|
w2conf |
wise_allskysc |
WISE |
Estimated confusion noise in the W2 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w2sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
ADU |
-0.9999995e9 |
|
w2conf |
wise_prelimsc |
WISE |
Estimated confusion noise in the W2 sky background annulus, in digital numbers This number is the difference between the measured noise in the sky background w2sigsk and the noise measured in the same region on the Atlas Uncertainty Maps |
float |
8 |
ADU |
-0.9999995e9 |
|
w2Cov |
catwise_2020, catwise_prelim |
WISE |
mean coverage depth, band-2 |
real |
4 |
|
|
|
w2cov |
allwise_sc |
WISE |
Mean pixel coverage in W2. This column gives the mean pixel value from the W2 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
float |
8 |
|
|
|
W2cov may differ from the integer frame coverage value given in w2m for two reasons. First, individual pixels in the measurement area may be masked or otherwise unusable, reducing the effective pixel count and thus the mean coverage value. Second, the effective sky area sampled by a pixels in single-exposure image varies across the focal plane because of field distortion. Distortion is corrected when coadding to generate the Atlas Images. Therefore, the effective number of pixels contributing to a pixel in the Atlas Coverage Map may be slightly smaller or larger than expected if there was no distortion. |
w2cov |
wise_allskysc |
WISE |
Mean pixel coverage in W2. This column gives the mean pixel value from the W2 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
real |
4 |
|
-0.9999995e9 |
|
w2cov |
wise_prelimsc |
WISE |
Mean pixel coverage in W2 This column gives the mean pixel value from the W2 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source |
real |
4 |
|
-0.9999995e9 |
|
w2dmag |
wise_allskysc |
WISE |
Difference between maximum and minimum magnitude of the source from all usable single-exposure frames, W2. Single-exposure measurements with w2rchi2 values greater than 3.0 times the median are rejected from this computation. |
real |
4 |
mag |
-0.9999995e9 |
|
w2fitr |
catwise_2020, catwise_prelim |
WISE |
fitting radius, band-2 (clipped at 999.99) |
real |
4 |
asec |
|
|
w2flg |
allwise_sc |
WISE |
W2 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg |
catwise_2020, catwise_prelim |
WISE |
standard aperture flag, band-2 |
int |
4 |
|
|
|
w2flg |
wise_allskysc |
WISE |
W2 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
smallint |
2 |
|
-9999 |
|
w2flg |
wise_prelimsc |
WISE |
W2 "standard" aperture measurement quality flag This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit |
smallint |
2 |
|
-9999 |
|
w2flg_1 |
allwise_sc |
WISE |
W2 5.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_1 |
wise_allskysc |
WISE |
W2 5.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_1 |
wise_prelimsc |
WISE |
W2 5.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_2 |
allwise_sc |
WISE |
W2 8.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_2 |
wise_allskysc |
WISE |
W2 8.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_2 |
wise_prelimsc |
WISE |
W2 8.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_3 |
allwise_sc |
WISE |
W2 11.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_3 |
wise_allskysc |
WISE |
W2 11.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_3 |
wise_prelimsc |
WISE |
W2 11.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_4 |
allwise_sc |
WISE |
W2 13.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_4 |
wise_allskysc |
WISE |
W2 13.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_4 |
wise_prelimsc |
WISE |
W2 13.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_5 |
allwise_sc |
WISE |
W2 16.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_5 |
wise_allskysc |
WISE |
W2 16.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_5 |
wise_prelimsc |
WISE |
W2 16.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_6 |
allwise_sc |
WISE |
W2 19.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_6 |
wise_allskysc |
WISE |
W2 19.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_6 |
wise_prelimsc |
WISE |
W2 19.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_7 |
allwise_sc |
WISE |
W2 22.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_7 |
wise_allskysc |
WISE |
W2 22.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_7 |
wise_prelimsc |
WISE |
W2 22.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flg_8 |
allwise_sc |
WISE |
W2 24.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2flg_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture flag, band-2 |
int |
4 |
|
|
|
w2flg_8 |
wise_allskysc |
WISE |
W2 24.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w2flg_8 |
wise_prelimsc |
WISE |
W2 24.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2flux |
allwise_sc |
WISE |
The "raw" W2 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w2flux |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux, band-2 |
real |
4 |
dn |
|
|
w2flux |
wise_allskysc |
WISE |
The "raw" W2 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w2flux |
wise_prelimsc |
WISE |
The "raw" W2 source flux measured in profile-fit photometry in units of digital numbers This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w2flux_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux, band-2 |
real |
4 |
dn |
|
|
w2frl |
wise_prelimsc |
WISE |
Fraction of W2 pixels affected by latents This column gives the fraction of all W2 pixels in the stack of individual W2 exposures used to characterize this source that may be affected by the presence of a latent image produced by a bright source |
real |
4 |
|
-0.9999995e9 |
|
w2frtr |
wise_allskysc |
WISE |
Fraction of W2 pixels affected by transients. This column gives the fraction of all W2 pixels in the stack of individual W2 exposures used to characterize this source that may be affected by transient events. This number is computed by counting the number of pixels in the single exposure Bit Mask images with value "21" that are present within the profile-fitting area, a circular region with radius of 7.25", centered on the position of this source, and dividing by the total number of pixels in the same area that are available for measurement. |
real |
4 |
|
-0.9999995e9 |
|
w2gerr |
allwise_sc |
WISE |
Uncertainty in the W2 magnitude of source measured in elliptical aperture. CAUTION: A w2gerr value of 9.999 indicates that the measurement uncertainty is very large, or the uncertainty could not be computed. In either case, the w2gmag measurement should be considered highly suspect. |
float |
8 |
mag |
|
|
w2gerr |
wise_allskysc |
WISE |
Uncertainty in the W2 magnitude of source measured in elliptical aperture. |
real |
4 |
mag |
-0.9999995e9 |
|
w2gerr |
wise_prelimsc |
WISE |
Uncertainty in the W2 magnitude of source measured in elliptical aperture |
real |
4 |
mag |
-0.9999995e9 |
|
w2gflg |
allwise_sc |
WISE |
W2 elliptical aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w2gflg |
wise_allskysc |
WISE |
W2 elliptical aperture measurement quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag, w2mflg. |
smallint |
2 |
|
-9999 |
|
w2gflg |
wise_prelimsc |
WISE |
W2 elliptical aperture measurement quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w2gmag |
allwise_sc |
WISE |
W2 magnitude of source measured in the elliptical aperture described by w2rsemi, w2ba, and w2pa. |
float |
8 |
mag |
|
|
w2gmag |
wise_allskysc |
WISE |
W2 magnitude of source measured in the elliptical aperture described by w2rsemi, w2ba, and w2pa. |
real |
4 |
mag |
-0.9999995e9 |
|
w2gmag |
wise_prelimsc |
WISE |
W2 magnitude of source measured in the elliptical aperture described by w2rsemi, w2ba, and w2pa |
real |
4 |
mag |
-0.9999995e9 |
|
w2k |
allwise_sc |
WISE |
Stetson K variability index (Stetson, P. 1996, PASP, 108, 851) computed using the W2 profile-fit fluxes measured on the individual single-exposure images. This column is null if there are <3 single-exposure measurements available in W2. |
float |
8 |
|
|
|
w2k |
catwise_2020, catwise_prelim |
WISE |
Stetson k index for variability; band-2 |
real |
4 |
|
|
|
w2M |
catwise_2020, catwise_prelim |
WISE |
WPRO, M , band-2 M == number of flux measurements for a given source |
int |
4 |
|
|
|
w2m |
allwise_sc |
WISE |
Integer frame coverage. This column gives the number of individual 7.7s W2 exposures on which a profile-fit measurement of this source was possible. This number can differ between the four bands because band-dependent criteria are used to select individual frames for inclusion in the coadded Atlas Images. This column is null if there is no frame coverage in this band at the position of this source. |
int |
4 |
|
|
|
w2m |
wise_allskysc |
WISE |
Integer frame coverage in W2. This column gives the number of individual 7.7s W2 exposures on which a profile-fit measurement of this source was possible. |
bigint |
8 |
|
-99999999 |
|
w2m |
wise_prelimsc |
WISE |
Integer frame coverage in W2 This column gives the number of individual 7.7s W2 exposures on which a profile-fit measurement of this source was possible |
bigint |
8 |
|
-99999999 |
|
w2mag |
allwise_sc |
WISE |
W2 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". The curve-of-growth correction is given in w2mcor. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag |
catwise_2020, catwise_prelim |
WISE |
standard aperture mag w/ correction applied |
real |
4 |
mag |
|
|
w2mag |
wise_allskysc |
WISE |
W2 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag |
wise_prelimsc |
WISE |
W2 "standard" aperture magnitude This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_1 |
allwise_sc |
WISE |
W2 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_1 |
wise_allskysc |
WISE |
W2 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_1 |
wise_prelimsc |
WISE |
W2 5.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_2 |
allwise_sc |
WISE |
W2 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_2 |
wise_allskysc |
WISE |
W2 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_2 |
wise_prelimsc |
WISE |
W2 8.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_3 |
allwise_sc |
WISE |
W2 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_3 |
wise_allskysc |
WISE |
W2 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_3 |
wise_prelimsc |
WISE |
W2 11.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_4 |
allwise_sc |
WISE |
W2 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_4 |
wise_allskysc |
WISE |
W2 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_4 |
wise_prelimsc |
WISE |
W2 13.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_5 |
allwise_sc |
WISE |
W2 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_5 |
wise_allskysc |
WISE |
W2 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_5 |
wise_prelimsc |
WISE |
W2 16.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_6 |
allwise_sc |
WISE |
W2 19.25" radius aperture magnitude. This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_6 |
wise_allskysc |
WISE |
W2 19.25" radius aperture magnitude This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag. |
-0.9999995e9 |
|
w2mag_6 |
wise_prelimsc |
WISE |
W2 19.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_7 |
allwise_sc |
WISE |
W2 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_7 |
wise_allskysc |
WISE |
W2 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_7 |
wise_prelimsc |
WISE |
W2 22.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_8 |
allwise_sc |
WISE |
W2 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W2. |
float |
8 |
mag |
|
|
w2mag_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture mag, band-2 |
real |
4 |
mag |
|
|
w2mag_8 |
wise_allskysc |
WISE |
W2 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W2. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mag_8 |
wise_prelimsc |
WISE |
W2 24.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W2 |
real |
4 |
mag |
-0.9999995e9 |
|
W2mag_ALLWISE |
ravedr5Source |
RAVE |
W2 magnitude from ALLWISE |
real |
4 |
mag |
|
phot.mag;em.opt |
w2magP |
catwise_2020, catwise_prelim |
WISE |
WPRO repeatability mag; band-2 |
real |
4 |
mag |
|
|
w2magp |
allwise_sc |
WISE |
Magnitude computed from the inverse-variance-weighted mean of the profile-fit flux measurements on the w2m individual W2 frames covering this source. This differs from w2mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w2mpro is computed by fitting all W2 frames simultaneously and incorporating a robust error model. This column is "null" if w2m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w2mpro for the optimal flux measurement for point sources. |
float |
8 |
mag |
|
|
w2magp |
wise_allskysc |
WISE |
Inverse-variance-weighted mean W2 magnitude computed from profile-fit measurements on the w2m individual frames covering this source. This differs from w2mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w2mpro is computed by fitting all W2 frames simultaneously and incorporating a robust error model. This column is default if w2m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w2mpro for the optimal flux measurement for point sources. |
real |
4 |
mag |
-0.9999995e9 |
|
w2magp |
wise_prelimsc |
WISE |
Inverse-variance-weighted mean W2 magnitude computed from profile-fit measurements on the w2m individual frames covering this source This differs from w2mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w2mpro is computed by fitting all W2 frames simultaneously and incorporating a robust error model. This column is default if w2m=0, the mean flux is negative or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mcor |
allwise_sc |
WISE |
W2 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w2mag_2, to give the "standard-aperture" magnitude. |
float |
8 |
mag |
|
|
w2mcor |
wise_allskysc |
WISE |
W2 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w2mag_2, to give the "standard-aperture" magnitude. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mcor |
wise_prelimsc |
WISE |
W2 aperture curve-of-growth correction, in magnitudes This correction is subtracted from the nominal 8.25" aperture photometry brightness, w2mag_2, to give the "standard-aperture" magnitude |
real |
4 |
mag |
-0.9999995e9 |
|
w2mCorr |
twompzPhotoz |
TWOMPZ |
WISE w2mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: W2mCorr} |
real |
4 |
mag |
-0.9999995e9 |
|
w2mCorr |
wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm |
WISExSCOSPZ |
WISE w2mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: W2C} |
real |
4 |
mag |
-0.9999995e9 |
|
w2mCorrErr |
twompzPhotoz |
TWOMPZ |
W2 profile fit photometric measurement uncertainty {image primary HDU keyword: w2sigmpro} |
real |
4 |
mag |
-0.9999995e9 |
|
w2mCorrErr |
wiseScosSvm |
WISExSCOSPZ |
Error on WISE w2mpro measurement corrected for Galactic dust extinction {image primary HDU keyword: w2sigmpro} |
real |
4 |
|
-0.9999995e9 |
|
w2mJDmax |
catwise_2020, catwise_prelim |
WISE |
maximum mJD; band-2 |
float |
8 |
|
|
|
w2mjdmax |
allwise_sc, wise_allskysc |
WISE |
The latest modified Julian Date (mJD) of the W2 single-exposures covering the source. |
float |
8 |
|
|
|
w2mJDmean |
catwise_2020, catwise_prelim |
WISE |
mean mJD; band-2 |
float |
8 |
|
|
|
w2mjdmean |
allwise_sc, wise_allskysc |
WISE |
The average modified Julian Date (mJD) of the W2 single-exposures covering the source. |
float |
8 |
|
|
|
w2mJDmin |
catwise_2020, catwise_prelim |
WISE |
minimum mJD; band-2 |
float |
8 |
|
|
|
w2mjdmin |
allwise_sc, wise_allskysc |
WISE |
The earliest modified Julian Date (mJD) of the W2 single-exposures covering the source. |
float |
8 |
|
|
|
w2mLQ |
catwise_2020, catwise_prelim |
WISE |
-log(Q), Q = 1-P(chi-square); band-2 |
real |
4 |
|
|
|
w2mlq |
allwise_sc |
WISE |
Probability measure that the source is variable in W2 flux. The value is -ln(Q), where Q = 1 - P(χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
float |
8 |
|
|
|
The Q value is the fraction of all cases to be at least as large as that observed if the null hypothesis is true. The null hypothesis is that the flux is emitted by a non-variable astrophysical object. It may be false because the object is a true variable. It may also be false because the flux measurement is corrupted by artifacts such as cosmic rays, scattered light, etc. The smaller the Q value, the more implausible the null hypothesis, i.e., the more likely it is that the flux is either variable or corrupted or both. |
w2mlq |
wise_allskysc |
WISE |
Probability measure that the source is variable in W2 flux. The value is -log10(Q), where Q = 1 - P(Χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
int |
4 |
|
-99999999 |
|
w2mpro |
allwise_sc |
WISE |
W2 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W2 flux measurement has SNR<2. This column is null if the source is nominally detected in W2, but no useful brightness estimate could be made. |
float |
8 |
mag |
|
|
w2mpro |
catwise_2020, catwise_prelim |
WISE |
WPRO flux in mag units, band-2 |
real |
4 |
mag |
|
|
w2mpro |
wise_allskysc |
WISE |
W2 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W2 flux measurement has SNR<2. This column is default if the source is nominally detected in W2, but no useful brightness estimate could be made. |
real |
4 |
mag |
-0.9999995e9 |
|
w2mpro |
wise_prelimsc |
WISE |
W2 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W2 flux measurement has SNR<2 This column is default if the source is nominally detected in W2, but no useful brightness estimate could be made |
real |
4 |
mag |
-0.9999995e9 |
|
w2mpro_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO flux in mag units, band-2 |
real |
4 |
mag |
|
|
w2Ndf |
catwise_2020, catwise_prelim |
WISE |
No. degrees of freedom in var chi-square; band-2 |
int |
4 |
|
|
|
w2ndf |
allwise_sc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W2. |
int |
4 |
|
|
|
w2ndf |
wise_allskysc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W2. |
bigint |
8 |
|
-99999999 |
|
w2NM |
catwise_2020, catwise_prelim |
WISE |
WPRO, N (of M), band-2 M == number of flux measurements for a given source; N == number of M sources that have SNR >= 3 |
int |
4 |
|
|
|
w2nm |
allwise_sc |
WISE |
Integer frame detection count. This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W2 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
int |
4 |
|
|
|
w2nm |
wise_allskysc |
WISE |
Integer frame detection count in W2. This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W2 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
bigint |
8 |
|
-99999999 |
|
w2nm |
wise_prelimsc |
WISE |
Integer frame detection count in W2 This column gives the number of individual 7.7s exposures on which this source was detected with SNR>3 in the W2 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures |
bigint |
8 |
|
-99999999 |
|
w2pa |
allwise_sc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W2. |
float |
8 |
deg |
|
|
w2pa |
wise_allskysc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W2. |
real |
4 |
degrees |
-0.9999995e9 |
|
w2pa |
wise_prelimsc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W2 |
real |
4 |
degrees |
-0.9999995e9 |
|
w2rchi2 |
allwise_sc |
WISE |
Reduced χ2 of the W2 profile-fit photometry measurement. This column is null if the W2 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
|
|
w2rchi2 |
catwise_2020, catwise_prelim |
WISE |
WPRO reduced chi^2, band-2 |
real |
4 |
|
|
|
w2rchi2 |
wise_allskysc |
WISE |
Reduced chi-squared of the W2 profile-fit photometry measurement. This column is default if the W2 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
-0.9999995e9 |
|
w2rchi2 |
wise_prelimsc |
WISE |
Reduced chi-squared of the W2 profile-fit photometry measurement This column is default if the W2 magnitude is a 95% confidence upper limit (i.e. the source is not detected) |
real |
4 |
|
-0.9999995e9 |
|
w2rchi2_pm |
allwise_sc |
WISE |
Reduced χ2 of the W2 profile-fit photometry measurement including motion estimation. This column is null if the source is not detected in W2 magnitude or if the motion fit failed to converge or was not attempted. |
real |
4 |
|
|
|
w2rchi2_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO reduced chi^2, band-2 |
real |
4 |
|
|
|
w2rsemi |
allwise_sc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W2. |
float |
8 |
arcsec |
|
|
w2rsemi |
wise_allskysc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W2. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w2rsemi |
wise_prelimsc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W2 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w2Sat |
catwise_2020, catwise_prelim |
WISE |
fraction of pixels saturated, band-2 |
real |
4 |
|
|
|
w2sat |
allwise_sc |
WISE |
Saturated pixel fraction, W2. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W2]~7 mag. Saturation may occur in fainter sources because of charged particle strikes. |
float |
8 |
|
|
|
w2sat |
wise_allskysc |
WISE |
Saturated pixel fraction, W2. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W2]∼7 mag. Saturation may occur in fainter sources because of a charged particle strike. |
real |
4 |
|
-0.9999995e9 |
|
w2sat |
wise_prelimsc |
WISE |
Saturated pixel fraction, W2 The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation |
real |
4 |
|
-0.9999995e9 |
|
w2sigflux |
allwise_sc |
WISE |
Uncertainty in the "raw" W2 source flux measurement in profile-fit photometry in units of digital numbers. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w2sigflux |
catwise_2020, catwise_prelim |
WISE |
WPRO raw flux uncertainty, band-2 |
real |
4 |
dn |
|
|
w2sigflux |
wise_allskysc |
WISE |
Uncertainty in the "raw" W2 source flux measurement in profile-fit photometry in units of digital numbers. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w2sigflux |
wise_prelimsc |
WISE |
Uncertainty in the "raw" W2 source flux measurement in profile-fit photometry in units of digital numbers This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w2sigflux_pm |
catwise_2020, catwise_prelim |
WISE |
fit WPRO raw flux uncertainty, band-2 |
real |
4 |
dn |
|
|
w2sigm |
allwise_sc |
WISE |
Uncertainty in the W2 "standard" aperture magnitude. This column is null if the W2 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm |
catwise_2020, catwise_prelim |
WISE |
standard aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm |
wise_allskysc |
WISE |
Uncertainty in the W2 "standard" aperture magnitude. This column is default if the W2 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm |
wise_prelimsc |
WISE |
Uncertainty in the W2 "standard" aperture magnitude This column is default if the W2 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_1 |
allwise_sc |
WISE |
Uncertainty in the W2 5.5" radius aperture magnitude. This column is null if the the 5.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_1 |
catwise_2020, catwise_prelim |
WISE |
Aper 1 (5.50 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_1 |
wise_allskysc |
WISE |
Uncertainty in the W2 5.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_1 |
wise_prelimsc |
WISE |
Uncertainty in the W2 5.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_2 |
allwise_sc |
WISE |
Uncertainty in the W2 8.25" radius aperture magnitude. This column is null if the the 8.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_2 |
catwise_2020, catwise_prelim |
WISE |
Aper 2 (8.25 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_2 |
wise_allskysc |
WISE |
Uncertainty in the W2 8.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_2 |
wise_prelimsc |
WISE |
Uncertainty in the W2 8.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_3 |
allwise_sc |
WISE |
Uncertainty in the W2 11.0" radius aperture magnitude. This column is null if the the 11.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_3 |
catwise_2020, catwise_prelim |
WISE |
Aper 3 (11.00 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_3 |
wise_allskysc |
WISE |
Uncertainty in the W2 11.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_3 |
wise_prelimsc |
WISE |
Uncertainty in the W2 11.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_4 |
allwise_sc |
WISE |
Uncertainty in the W2 13.75" radius aperture magnitude. This column is null if the the 13.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_4 |
catwise_2020, catwise_prelim |
WISE |
Aper 4 (13.75 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_4 |
wise_allskysc |
WISE |
Uncertainty in the W2 13.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_4 |
wise_prelimsc |
WISE |
Uncertainty in the W2 13.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_5 |
allwise_sc |
WISE |
Uncertainty in the W2 16.5" radius aperture magnitude. This column is null if the the 16.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_5 |
catwise_2020, catwise_prelim |
WISE |
Aper 5 (16.50 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_5 |
wise_allskysc |
WISE |
Uncertainty in the W2 16.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_5 |
wise_prelimsc |
WISE |
Uncertainty in the W2 16.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_6 |
allwise_sc |
WISE |
Uncertainty in the W2 19.25" radius aperture magnitude. This column is null if the the 19.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_6 |
catwise_2020, catwise_prelim |
WISE |
Aper 6 (19.25 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_6 |
wise_allskysc |
WISE |
Uncertainty in the W2 19.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_6 |
wise_prelimsc |
WISE |
Uncertainty in the W2 19.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_7 |
allwise_sc |
WISE |
Uncertainty in the W2 22.0" radius aperture magnitude. This column is null if the the 22.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_7 |
catwise_2020, catwise_prelim |
WISE |
Aper 7 (22.00 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_7 |
wise_allskysc |
WISE |
Uncertainty in the W2 22.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_7 |
wise_prelimsc |
WISE |
Uncertainty in the W2 22.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_8 |
allwise_sc |
WISE |
Uncertainty in the W2 24.75" radius aperture magnitude. This column is null if the the 24.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w2sigm_8 |
catwise_2020, catwise_prelim |
WISE |
Aper 8 (24.75 arcsec), aperture mag uncertainty, band-2 |
real |
4 |
mag |
|
|
w2sigm_8 |
wise_allskysc |
WISE |
Uncertainty in the W2 24.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigm_8 |
wise_prelimsc |
WISE |
Uncertainty in the W2 24.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigmpro |
allwise_sc |
WISE |
W2 profile-fit photometric measurement uncertainty in mag units. This column is null if the W2 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
float |
8 |
mag |
|
|
w2sigmpro |
catwise_2020, catwise_prelim |
WISE |
WPRO flux uncertainty in mag units, band-2 |
real |
4 |
mag |
|
|
w2sigmpro |
wise_allskysc |
WISE |
W2 profile-fit photometric measurement uncertainty. This column is default if the W2 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigmpro |
wise_prelimsc |
WISE |
W2 profile-fit photometric measurement uncertainty This column is default if the W2 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigmpro_pm |
catwise_2020, catwise_prelim |
WISE |
WPRO flux uncertainty in mag units, band-2 |
real |
4 |
mag |
|
|
w2sigP1 |
catwise_2020, catwise_prelim |
WISE |
WPRO mag population sigma; band-2 |
real |
4 |
mag |
|
|
w2sigp1 |
allwise_sc |
WISE |
Standard deviation of the population of W2 fluxes measured on the w2m individual frames covering this source, in magnitudes. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is "null" if w2m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w2sigp1 |
wise_allskysc |
WISE |
Standard deviation of the population of W2 fluxes measured on the w2m individual frames covering this source. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w2m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigp1 |
wise_prelimsc |
WISE |
Standard deviation of the population of W2 fluxes measured on the w2m individual frames covering this source This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w2m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigP2 |
catwise_2020, catwise_prelim |
WISE |
WPRO mag uncertainty of the mean; band-2 |
real |
4 |
mag |
|
|
w2sigp2 |
allwise_sc |
WISE |
Standard deviation of the mean of the distribution of W2 fluxes (w2magp) computed from profile-fit measurements on the w2m individual frames covering this source, in magnitudes. This is equivalent to w2sigp1/sqrt(w2m). This column is "null" if w2m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w2sigp2 |
wise_allskysc |
WISE |
Standard deviation of the mean of the distribution of W2 fluxes (w2magp) computed from profile-fit measurements on the w2m individual frames covering this source. This column is default if w2m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigp2 |
wise_prelimsc |
WISE |
Standard deviation of the mean of the distribution of W2 fluxes (w2magp) computed from profile-fit measurements on the w2m individual frames covering this source This column is default if w2m<2 or if no individual frame measurements are possible |
real |
4 |
mag |
-0.9999995e9 |
|
w2sigsk |
allwise_sc |
WISE |
The uncertainty in the W2 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
float |
8 |
dn |
|
|
w2sigsk |
catwise_2020, catwise_prelim |
WISE |
frame sky background value uncertainty, band-2 |
real |
4 |
dn |
|
|
w2sigsk |
wise_allskysc |
WISE |
The uncertainty in the W2 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
real |
4 |
ADU |
-0.9999995e9 |
|
w2sigsk |
wise_prelimsc |
WISE |
The uncertainty in the W2 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" |
real |
4 |
ADU |
-0.9999995e9 |
|
w2sky |
allwise_sc |
WISE |
The trimmed average of the W2 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
dn |
|
|
For profile-fit photometry, the sky background is measured on the individual single-exposure images that are used for source characterization. For aperture photometry, the sky background is measured on the Atlas Image. |
w2sky |
catwise_2020, catwise_prelim |
WISE |
frame sky background value, band-2 |
real |
4 |
dn |
|
|
w2sky |
wise_allskysc |
WISE |
The trimmed average of the W2 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
ADU |
-0.9999995e9 |
|
w2sky |
wise_prelimsc |
WISE |
The trimmed average of the W2 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value |
float |
8 |
ADU |
-0.9999995e9 |
|
w2snr |
allwise_sc |
WISE |
W2 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w2flux) to flux uncertainty (w2sigflux)in the W2 profile-fit photometry measurement. This column is null if w2flux is negative, or if w2flux or w2sigflux are null. |
float |
8 |
|
|
|
w2snr |
catwise_2020, catwise_prelim |
WISE |
S/N ratio, band-2 |
real |
4 |
|
|
|
w2snr |
wise_allskysc |
WISE |
W2 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w2flux) to flux uncertainty (w2sigflux) in the W2 profile-fit photometry measurement. This column is default if w2flux is negative, or if w2flux or w2sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w2snr |
wise_prelimsc |
WISE |
W2 profile-fit measurement signal-to-noise ratio This value is the ratio of the flux (w2flux) to flux uncertainty (w2sigflux)in the W2 profile-fit photometry measurement. This column is default if w2flux is negative, or if w2flux or w2sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w2snr_pm |
catwise_2020, catwise_prelim |
WISE |
flux S/N ratio, band-2 |
real |
4 |
|
|
|
w3ba |
allwise_sc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W3. |
float |
8 |
arcsec |
|
|
w3ba |
wise_allskysc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W3. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w3ba |
wise_prelimsc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W3 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w3cc_map |
allwise_sc |
WISE |
Contamination and confusion map for this source in W3. This column contains the integer equivalent of the 9-bit binary number that specifies if the W3 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
int |
4 |
|
|
|
The elements of the binary array are: S 0 0 0 O H 0 P D. The leftmost bit, S, differentiates whether the band-detection is believed to be a real detection contaminated by an artifact ("0") or a spurious detection of an artifact ("1"). The remaining bits are set to "1" to denote contamination by different types of artifacts according to the letters: - D - Diffraction spike. Source may be a spurious detection of or contaminated by a diffraction spike of a nearby bright star on the same image.
- P - Persistence. Source may be a spurious detection of or contaminated by a short-term latent (persistence) image left by a bright source.
- H - Halo. Source may be a spurious detection of or contaminated by the scattered light halo associated with a bright star.
- O (letter "o") - Optical ghost. Source may be a spurious detection of or contaminated by an optical ghost image caused by a nearby bright source on the same image.
For example, a measurement that is believed to be a spurious detection of a diffraction spike and scattered light halo has a binary bit map value of "100001001" and w?cc_map=265. |
w3cc_map |
wise_allskysc |
WISE |
Contamination and confusion map for this source in W3. This column contains the integer equivalent of the 9-bit binary number that specifies if the W3 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
smallint |
2 |
|
|
|
w3cc_map |
wise_prelimsc |
WISE |
Contamination and confusion map for this source in W3 This column contains the integer equivalent of the 9-bit binary number that specifies if the W3 measurement is believed to be contaminated by or a spurious detection of an image artifact |
smallint |
2 |
|
|
|
w3cc_map_str |
allwise_sc |
WISE |
Contamination and confusion string. This column is a character string that denotes all artifacts that may contaminate the W3 measurement of this source, in the priority order D,P,H,O,d,p,h,o. Lower-case letters denote cases where the source detection in this band is believed to be real but the measurement may be contaminated by the artifact. Upper-case letters denote cases where the source detection in this band may be a spurious detection of an artifact. This string is "null" if there are no artifacts that affect the measurement in this band. The value that appears in third element of the cc_flags string is the left-most character in w3cc_map_str. If w3cc_map_str is "null", then the corresponding cc_flags entry is "0". |
varchar |
9 |
|
|
|
For example, a real detection that is contaminated by a diffraction spike and a latent (persistent) image has a w?cc_map_str="dp". A spurious detection of a diffraction spike that is also contaminated by a latent image has w?cc_map_str="Dp". |
w3cc_map_str |
wise_allskysc |
WISE |
Contamination and confusion string in W3. This column is a character string that denotes all artifacts that may contaminate the W3 measurement of this source, in the priority order D,P,H,O,d,p,h,o. |
char |
9 |
|
|
|
w3cc_map_str |
wise_prelimsc |
WISE |
Contamination and confusion string in W3 This column is a character string that denotes all artifacts that may contaminate the W3 measurement of this source, in the priority order D,P,H,O |
char |
9 |
|
|
|
w3conf |
allwise_sc |
WISE |
Estimated confusion noise in the W3 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w3sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
dn |
|
|
w3conf |
wise_allskysc |
WISE |
Estimated confusion noise in the W3 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w3sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
ADU |
-0.9999995e9 |
|
w3conf |
wise_prelimsc |
WISE |
Estimated confusion noise in the W3 sky background annulus, in digital numbers This number is the difference between the measured noise in the sky background w3sigsk and the noise measured in the same region on the Atlas Uncertainty Maps |
float |
8 |
ADU |
-0.9999995e9 |
|
w3cov |
allwise_sc |
WISE |
Mean pixel coverage in W3. This column gives the mean pixel value from the W3 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
float |
8 |
|
|
|
W3cov may differ from the integer frame coverage value given in w3m for two reasons. First, individual pixels in the measurement area may be masked or otherwise unusable, reducing the effective pixel count and thus the mean coverage value. Second, the effective sky area sampled by a pixels in single-exposure image varies across the focal plane because of field distortion. Distortion is corrected when coadding to generate the Atlas Images. Therefore, the effective number of pixels contributing to a pixel in the Atlas Coverage Map may be slightly smaller or larger than expected if there was no distortion. |
w3cov |
wise_allskysc |
WISE |
Mean pixel coverage in W3. This column gives the mean pixel value from the W3 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source. |
real |
4 |
|
-0.9999995e9 |
|
w3cov |
wise_prelimsc |
WISE |
Mean pixel coverage in W3 This column gives the mean pixel value from the W3 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 8.25" centered on the position of this source |
real |
4 |
|
-0.9999995e9 |
|
w3dmag |
wise_allskysc |
WISE |
Difference between maximum and minimum magnitude of the source from all usable single-exposure frames, W3. Single-exposure measurements with w3rchi2 values greater than 3.0 times the median are rejected from this computation. |
real |
4 |
mag |
-0.9999995e9 |
|
w3flg |
allwise_sc |
WISE |
W3 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg |
wise_allskysc |
WISE |
W3 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
smallint |
2 |
|
-9999 |
|
w3flg |
wise_prelimsc |
WISE |
W3 "standard" aperture measurement quality flag This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit |
smallint |
2 |
|
-9999 |
|
w3flg_1 |
allwise_sc |
WISE |
W3 5.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_1 |
wise_allskysc |
WISE |
W3 5.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_1 |
wise_prelimsc |
WISE |
W3 5.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_2 |
allwise_sc |
WISE |
W3 8.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_2 |
wise_allskysc |
WISE |
W3 8.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_2 |
wise_prelimsc |
WISE |
W3 8.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_3 |
allwise_sc |
WISE |
W3 11.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_3 |
wise_allskysc |
WISE |
W3 11.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_3 |
wise_prelimsc |
WISE |
W3 11.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_4 |
allwise_sc |
WISE |
W3 13.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_4 |
wise_allskysc |
WISE |
W3 13.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_4 |
wise_prelimsc |
WISE |
W3 13.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_5 |
allwise_sc |
WISE |
W3 16.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_5 |
wise_allskysc |
WISE |
W3 16.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_5 |
wise_prelimsc |
WISE |
W3 16.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_6 |
allwise_sc |
WISE |
W3 19.25" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_6 |
wise_allskysc |
WISE |
W3 19.25" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_6 |
wise_prelimsc |
WISE |
W3 19.25" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_7 |
allwise_sc |
WISE |
W3 22.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_7 |
wise_allskysc |
WISE |
W3 22.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_7 |
wise_prelimsc |
WISE |
W3 22.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flg_8 |
allwise_sc |
WISE |
W3 24.75" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3flg_8 |
wise_allskysc |
WISE |
W3 24.75" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w3flg_8 |
wise_prelimsc |
WISE |
W3 24.75" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3flux |
allwise_sc |
WISE |
The "raw" W3 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w3flux |
wise_allskysc |
WISE |
The "raw" W3 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w3flux |
wise_prelimsc |
WISE |
The "raw" W3 source flux measured in profile-fit photometry in units of digital numbers This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w3frl |
wise_prelimsc |
WISE |
Fraction of W3 pixels affected by latents This column gives the fraction of all W3 pixels in the stack of individual W3 exposures used to characterize this source that may be affected by the presence of a latent image produced by a bright source |
real |
4 |
|
-0.9999995e9 |
|
w3frtr |
wise_allskysc |
WISE |
Fraction of W3 pixels affected by transients. This column gives the fraction of all W3 pixels in the stack of individual W3 exposures used to characterize this source that may be affected by transient events. This number is computed by counting the number of pixels in the single exposure Bit Mask images with value "21" that are present within the profile-fitting area, a circular region with radius of 7.25", centered on the position of this source, and dividing by the total number of pixels in the same area that are available for measurement. |
real |
4 |
|
-0.9999995e9 |
|
w3gerr |
allwise_sc |
WISE |
Uncertainty in the W3 magnitude of source measured in elliptical aperture. CAUTION: A w3gerr value of 9.999 indicates that the measurement uncertainty is very large, or the uncertainty could not be computed. In either case, the w3gmag measurement should be considered highly suspect. |
float |
8 |
mag |
|
|
w3gerr |
wise_allskysc |
WISE |
Uncertainty in the W3 magnitude of source measured in elliptical aperture. |
real |
4 |
mag |
-0.9999995e9 |
|
w3gerr |
wise_prelimsc |
WISE |
Uncertainty in the W3 magnitude of source measured in elliptical aperture |
real |
4 |
mag |
-0.9999995e9 |
|
w3gflg |
allwise_sc |
WISE |
W3 elliptical aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w3gflg |
wise_allskysc |
WISE |
W3 elliptical aperture measurement quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag, w3mflg. |
smallint |
2 |
|
-9999 |
|
w3gflg |
wise_prelimsc |
WISE |
W3 elliptical aperture measurement quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w3gmag |
allwise_sc |
WISE |
W3 magnitude of source measured in the elliptical aperture described by w3rsemi, w3ba, and w3pa. |
float |
8 |
mag |
|
|
w3gmag |
wise_allskysc |
WISE |
W3 magnitude of source measured in the elliptical aperture described by w3rsemi, w3ba, and w3pa. |
real |
4 |
mag |
-0.9999995e9 |
|
w3gmag |
wise_prelimsc |
WISE |
W3 magnitude of source measured in the elliptical aperture described by w3rsemi, w3ba, and w3pa |
real |
4 |
mag |
-0.9999995e9 |
|
w3k |
allwise_sc |
WISE |
Stetson K variability index (Stetson, P. 1996, PASP, 108, 851) computed using the W3 profile-fit fluxes measured on the individual single-exposure images. This column is null if there are <3 single-exposure measurements available in W3. |
float |
8 |
|
|
|
w3m |
allwise_sc |
WISE |
Integer frame coverage. This column gives the number of individual 8.8s W3 exposures on which a profile-fit measurement of this source was possible. This number can differ between the four bands because band-dependent criteria are used to select individual frames for inclusion in the coadded Atlas Images. This column is null if there is no frame coverage in this band at the position of this source. |
int |
4 |
|
|
|
w3m |
wise_allskysc |
WISE |
Integer frame coverage in W3. This column gives the number of individual 8.8s W3 exposures on which a profile-fit measurement of this source was possible. |
bigint |
8 |
|
-99999999 |
|
w3m |
wise_prelimsc |
WISE |
Integer frame coverage in W3 This column gives the number of individual 8.8s W3 exposures on which a profile-fit measurement of this source was possible. |
bigint |
8 |
|
-99999999 |
|
w3mag |
allwise_sc |
WISE |
W3 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". The curve-of-growth correction is given in w3mcor. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag |
wise_allskysc |
WISE |
W3 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag |
wise_prelimsc |
WISE |
W3 "standard" aperture magnitude This is the curve-of-growth corrected source brightness measured in an 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_1 |
allwise_sc |
WISE |
W3 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_1 |
wise_allskysc |
WISE |
W3 5.5" radius aperture magnitude. This is the calibrated source brightness measured in a 5.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_1 |
wise_prelimsc |
WISE |
W3 5.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_2 |
allwise_sc |
WISE |
W3 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_2 |
wise_allskysc |
WISE |
W3 8.25" radius aperture magnitude. This is the calibrated source brightness measured in a 8.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_2 |
wise_prelimsc |
WISE |
W3 8.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_3 |
allwise_sc |
WISE |
W3 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_3 |
wise_allskysc |
WISE |
W3 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_3 |
wise_prelimsc |
WISE |
W3 11.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_4 |
allwise_sc |
WISE |
W3 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_4 |
wise_allskysc |
WISE |
W3 13.75" radius aperture magnitude. This is the calibrated source brightness measured in a 13.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag. |
-0.9999995e9 |
|
w3mag_4 |
wise_prelimsc |
WISE |
W3 13.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_5 |
allwise_sc |
WISE |
W3 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_5 |
wise_allskysc |
WISE |
W3 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_5 |
wise_prelimsc |
WISE |
W3 16.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_6 |
allwise_sc |
WISE |
W3 19.25" radius aperture magnitude. This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_6 |
wise_allskysc |
WISE |
W3 19.25" radius aperture magnitude. This is the calibrated source brightness measured in a 19.25" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_6 |
wise_prelimsc |
WISE |
W3 19.25" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_7 |
allwise_sc |
WISE |
W3 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_7 |
wise_allskysc |
WISE |
W3 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_7 |
wise_prelimsc |
WISE |
W3 22.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_8 |
allwise_sc |
WISE |
W3 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W3. |
float |
8 |
mag |
|
|
w3mag_8 |
wise_allskysc |
WISE |
W3 24.75" radius aperture magnitude. This is the calibrated source brightness measured in a 24.75" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W3. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mag_8 |
wise_prelimsc |
WISE |
W3 24.75" radius aperture magnitude This column is default if this aperture measurement was not possible in W3 |
real |
4 |
mag |
-0.9999995e9 |
|
W3mag_ALLWISE |
ravedr5Source |
RAVE |
W3 magnitude from ALLWISE |
real |
4 |
mag |
|
phot.mag;em.opt |
w3magp |
allwise_sc |
WISE |
Magnitude computed from the inverse-variance-weighted mean of the profile-fit flux measurements on the w3m individual W3 frames covering this source. This differs from w3mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w3mpro is computed by fitting all W3 frames simultaneously and incorporating a robust error model. This column is "null" if w3m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w3mpro for the optimal flux measurement for point sources. |
float |
8 |
mag |
|
|
w3magp |
wise_allskysc |
WISE |
Inverse-variance-weighted mean W3 magnitude computed from profile-fit measurements on the w3m individual frames covering this source. This differs from w3mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w3mpro is computed by fitting all W3 frames simultaneously and incorporating a robust error model. This column is default if w3m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w3mpro for the optimal flux measurement for point sources. |
real |
4 |
mag |
-0.9999995e9 |
|
w3magp |
wise_prelimsc |
WISE |
Inverse-variance-weighted mean W3 magnitude computed from profile-fit measurements on the w3m individual frames covering this source This differs from w3mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w3mpro is computed by fitting all W3 frames simultaneously and incorporating a robust error model. This column is default if w3m=0, the mean flux is negative or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mcor |
allwise_sc |
WISE |
W3 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w3mag_2, to give the "standard-aperture" magnitude. |
float |
8 |
mag |
|
|
w3mcor |
wise_allskysc |
WISE |
W3 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 8.25" aperture photometry brightness, w3mag_2, to give the "standard-aperture" magnitude. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mcor |
wise_prelimsc |
WISE |
W3 aperture curve-of-growth correction, in magnitudes This correction is subtracted from the nominal 8.25" aperture photometry brightness, w3mag_2, to give the "standard-aperture" magnitude |
real |
4 |
mag |
-0.9999995e9 |
|
w3mjdmax |
allwise_sc, wise_allskysc |
WISE |
The latest modified Julian Date (mJD) of the W3 single-exposures covering the source. |
float |
8 |
|
|
|
w3mjdmean |
allwise_sc, wise_allskysc |
WISE |
The average modified Julian Date (mJD) of the W3 single-exposures covering the source. |
float |
8 |
|
|
|
w3mjdmin |
allwise_sc, wise_allskysc |
WISE |
The earliest modified Julian Date (mJD) of the W3 single-exposures covering the source. |
float |
8 |
|
|
|
w3mlq |
allwise_sc |
WISE |
Probability measure that the source is variable in W3 flux. The value is -ln(Q), where Q = 1 - P(χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
float |
8 |
|
|
|
The Q value is the fraction of all cases to be at least as large as that observed if the null hypothesis is true. The null hypothesis is that the flux is emitted by a non-variable astrophysical object. It may be false because the object is a true variable. It may also be false because the flux measurement is corrupted by artifacts such as cosmic rays, scattered light, etc. The smaller the Q value, the more implausible the null hypothesis, i.e., the more likely it is that the flux is either variable or corrupted or both. |
w3mlq |
wise_allskysc |
WISE |
Probability measure that the source is variable in W3 flux. The value is -log10(Q), where Q = 1 - P(Χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
int |
4 |
|
-99999999 |
|
w3mpro |
allwise_sc |
WISE |
W3 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W3 flux measurement has SNR<2. This column is null if the source is nominally detected in W3, but no useful brightness estimate could be made. |
float |
8 |
mag |
|
|
w3mpro |
wise_allskysc |
WISE |
W3 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W3 flux measurement has SNR<2. This column is default if the source is nominally detected in W3, but no useful brightness estimate could be made. |
real |
4 |
mag |
-0.9999995e9 |
|
w3mpro |
wise_prelimsc |
WISE |
W3 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W3 flux measurement has SNR<2 This column is default if the source is nominally detected in W3, but no useful brightness estimate could be made |
real |
4 |
mag |
-0.9999995e9 |
|
w3ndf |
allwise_sc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W3. |
int |
4 |
|
|
|
w3ndf |
wise_allskysc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W3. |
bigint |
8 |
|
-99999999 |
|
w3nm |
allwise_sc |
WISE |
Integer frame detection count. This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W3 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
int |
4 |
|
|
|
w3nm |
wise_allskysc |
WISE |
Integer frame detection count in W3. This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W3 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
bigint |
8 |
|
-99999999 |
|
w3nm |
wise_prelimsc |
WISE |
Integer frame detection count in W3 This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W3 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures |
bigint |
8 |
|
-99999999 |
|
w3pa |
allwise_sc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W3. |
float |
8 |
deg |
|
|
w3pa |
wise_allskysc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W3. |
real |
4 |
degrees |
-0.9999995e9 |
|
w3pa |
wise_prelimsc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W3 |
real |
4 |
degrees |
-0.9999995e9 |
|
w3rchi2 |
allwise_sc |
WISE |
Reduced χ2 of the W3 profile-fit photometry measurement. This column is null if the W3 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
|
|
w3rchi2 |
wise_allskysc |
WISE |
Reduced chi-squared of the W3 profile-fit photometry measurement. This column is default if the W3 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
-0.9999995e9 |
|
w3rchi2 |
wise_prelimsc |
WISE |
Reduced chi-squared of the W3 profile-fit photometry measurement This column is default if the W3 magnitude is a 95% confidence upper limit (i.e. the source is not detected) |
real |
4 |
|
-0.9999995e9 |
|
w3rchi2_pm |
allwise_sc |
WISE |
Reduced χ2 of the W3 profile-fit photometry measurement including motion estimation. This column is null if the source is not detected in W3 or if the motion fit failed to converge or was not attempted. |
real |
4 |
|
|
|
w3rsemi |
allwise_sc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W3. |
float |
8 |
arcsec |
|
|
w3rsemi |
wise_allskysc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W3. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w3rsemi |
wise_prelimsc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W3 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w3sat |
allwise_sc |
WISE |
Saturated pixel fraction, W3. The fraction of all pixels within the profile-fitting area source in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W3]~4 mag. Saturation may occur in fainter sources because of charged particle strikes. |
float |
8 |
|
|
|
w3sat |
wise_allskysc |
WISE |
Saturated pixel fraction, W3. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W3]~4 mag. Saturation may occur in fainter sources because of a charged particle strike. |
real |
4 |
|
-0.9999995e9 |
|
w3sat |
wise_prelimsc |
WISE |
Saturated pixel fraction, W3 The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation |
real |
4 |
|
-0.9999995e9 |
|
w3sigflux |
allwise_sc |
WISE |
Uncertainty in the "raw" W3 source flux measurement in profile-fit photometry in units of digital numbers. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w3sigflux |
wise_allskysc |
WISE |
Uncertainty in the "raw" W3 source flux measurement in profile-fit photometry in units of digital numbers. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w3sigflux |
wise_prelimsc |
WISE |
Uncertainty in the "raw" W3 source flux measurement in profile-fit photometry in units of digital numbers This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w3sigm |
allwise_sc |
WISE |
Uncertainty in the W3 "standard" aperture magnitude. This column is null if the W3 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm |
wise_allskysc |
WISE |
Uncertainty in the W3 "standard" aperture magnitude. This column is default if the W3 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm |
wise_prelimsc |
WISE |
Uncertainty in the W3 "standard" aperture magnitude This column is default if the W3 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_1 |
allwise_sc |
WISE |
Uncertainty in the W3 5.5" radius aperture magnitude. This column is null if the the 5.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_1 |
wise_allskysc |
WISE |
Uncertainty in the W3 5.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_1 |
wise_prelimsc |
WISE |
Uncertainty in the W3 5.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_2 |
allwise_sc |
WISE |
Uncertainty in the W3 8.25" radius aperture magnitude. This column is null if the the 8.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_2 |
wise_allskysc |
WISE |
Uncertainty in the W3 8.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_2 |
wise_prelimsc |
WISE |
Uncertainty in the W3 8.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_3 |
allwise_sc |
WISE |
Uncertainty in the W3 11.0" radius aperture magnitude. This column is null if the the 11.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_3 |
wise_allskysc |
WISE |
Uncertainty in the W3 11.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_3 |
wise_prelimsc |
WISE |
Uncertainty in the W3 11.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_4 |
allwise_sc |
WISE |
Uncertainty in the W3 13.75" radius aperture magnitude. This column is null if the the 13.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_4 |
wise_allskysc |
WISE |
Uncertainty in the W3 13.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_4 |
wise_prelimsc |
WISE |
Uncertainty in the W3 13.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_5 |
allwise_sc |
WISE |
Uncertainty in the W3 16.5" radius aperture magnitude. This column is null if the the 16.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_5 |
wise_allskysc |
WISE |
Uncertainty in the W3 16.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_5 |
wise_prelimsc |
WISE |
Uncertainty in the W3 16.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_6 |
allwise_sc |
WISE |
Uncertainty in the W3 19.25" radius aperture magnitude. This column is null if the the 19.25" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_6 |
wise_allskysc |
WISE |
Uncertainty in the W3 19.25" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_6 |
wise_prelimsc |
WISE |
Uncertainty in the W3 19.25" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_7 |
allwise_sc |
WISE |
Uncertainty in the W3 22.0" radius aperture magnitude. This column is null if the the 22.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_7 |
wise_allskysc |
WISE |
Uncertainty in the W3 22.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_7 |
wise_prelimsc |
WISE |
Uncertainty in the W3 22.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_8 |
allwise_sc |
WISE |
Uncertainty in the W3 24.75" radius aperture magnitude. This column is null if the the 24.75" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w3sigm_8 |
wise_allskysc |
WISE |
Uncertainty in the W3 24.75" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigm_8 |
wise_prelimsc |
WISE |
Uncertainty in the W3 24.75" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigmpro |
allwise_sc |
WISE |
W3 profile-fit photometric measurement uncertainty in mag units. This column is null if the W3 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
float |
8 |
mag |
|
|
w3sigmpro |
wise_allskysc |
WISE |
W3 profile-fit photometric measurement uncertainty. This column is default if the W3 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigmpro |
wise_prelimsc |
WISE |
W3 profile-fit photometric measurement uncertainty This column is default if the W3 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigp1 |
allwise_sc |
WISE |
Standard deviation of the population of W3 fluxes measured on the w3m individual frames covering this source, in magnitudes. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is "null" if w3m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w3sigp1 |
wise_allskysc |
WISE |
Standard deviation of the population of W3 fluxes measured on the w3m individual frames covering this source. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w3m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigp1 |
wise_prelimsc |
WISE |
Standard deviation of the population of W3 fluxes measured on the w3m individual frames covering this source This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w3m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigp2 |
allwise_sc |
WISE |
Standard deviation of the mean of the distribution of W3 fluxes (w3magp) computed from profile-fit measurements on the w3m individual frames covering this source, in magnitudes. This is equivalent to w3sigp1/sqrt(w3m). This column is "null" if w3m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w3sigp2 |
wise_allskysc |
WISE |
Standard deviation of the mean of the distribution of W3 fluxes (w3magp) computed from profile-fit measurements on the w3m individual frames covering this source. This column is default if w3m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigp2 |
wise_prelimsc |
WISE |
Standard deviation of the mean of the distribution of W3 fluxes (w3magp) computed from profile-fit measurements on the w3m individual frames covering this source This column is default if w3m<2 or if no individual frame measurements are possible |
real |
4 |
mag |
-0.9999995e9 |
|
w3sigsk |
allwise_sc |
WISE |
The uncertainty in the W3 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
float |
8 |
dn |
|
|
w3sigsk |
wise_allskysc |
WISE |
The uncertainty in the W3 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
real |
4 |
ADU |
-0.9999995e9 |
|
w3sigsk |
wise_prelimsc |
WISE |
The uncertainty in the W3 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" |
real |
4 |
ADU |
-0.9999995e9 |
|
w3sky |
allwise_sc |
WISE |
The trimmed average of the W3 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
dn |
|
|
For profile-fit photometry, the sky background is measured on the individual single-exposure images that are used for source characterization. For aperture photometry, the sky background is measured on the Atlas Image. |
w3sky |
wise_allskysc |
WISE |
The trimmed average of the W3 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
ADU |
-0.9999995e9 |
|
w3sky |
wise_prelimsc |
WISE |
The trimmed average of the W3 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value |
float |
8 |
ADU |
-0.9999995e9 |
|
w3snr |
allwise_sc |
WISE |
W3 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w3flux) to flux uncertainty (w3sigflux)in the W3 profile-fit photometry measurement. This column is null if w3flux is negative, or if w3flux or w3sigflux are null. |
float |
8 |
|
|
|
w3snr |
wise_allskysc |
WISE |
W3 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w3flux) to flux uncertainty (w3sigflux) in the W3 profile-fit photometry measurement. This column is default if w3flux is negative, or if w3flux or w3sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w3snr |
wise_prelimsc |
WISE |
W3 profile-fit measurement signal-to-noise ratio This value is the ratio of the flux (w3flux) to flux uncertainty (w3sigflux)in the W3 profile-fit photometry measurement. This column is default if w3flux is negative, or if w3flux or w3sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
W420F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 420/30 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W462F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 462/14 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W485F_D |
combo17CDFSSource |
COMBO17 |
flux in filter 485/31 in run D (07.10.-22.10.1999) |
float |
8 |
|
|
|
w4ba |
allwise_sc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W4. |
float |
8 |
arcsec |
|
|
w4ba |
wise_allskysc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W4. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w4ba |
wise_prelimsc |
WISE |
Axis ratio (b/a) of the elliptical aperture used to measure source in W4 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w4cc_map |
allwise_sc |
WISE |
Contamination and confusion map for this source in W4. This column contains the integer equivalent of the 9-bit binary number that specifies if the W4 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
int |
4 |
|
|
|
The elements of the binary array are: S 0 0 0 O H 0 P D. The leftmost bit, S, differentiates whether the band-detection is believed to be a real detection contaminated by an artifact ("0") or a spurious detection of an artifact ("1"). The remaining bits are set to "1" to denote contamination by different types of artifacts according to the letters: - D - Diffraction spike. Source may be a spurious detection of or contaminated by a diffraction spike of a nearby bright star on the same image.
- P - Persistence. Source may be a spurious detection of or contaminated by a short-term latent (persistence) image left by a bright source.
- H - Halo. Source may be a spurious detection of or contaminated by the scattered light halo associated with a bright star.
- O (letter "o") - Optical ghost. Source may be a spurious detection of or contaminated by an optical ghost image caused by a nearby bright source on the same image.
For example, a measurement that is believed to be a spurious detection of a diffraction spike and scattered light halo has a binary bit map value of "100001001" and w?cc_map=265. |
w4cc_map |
wise_allskysc |
WISE |
Contamination and confusion map for this source in W4. This column contains the integer equivalent of the 9-bit binary number that specifies if the W4 measurement is believed to be contaminated by or a spurious detection of an image artifact. |
smallint |
2 |
|
|
|
w4cc_map |
wise_prelimsc |
WISE |
Contamination and confusion map for this source in W4 This column contains the integer equivalent of the 9-bit binary number that specifies if the W4 measurement is believed to be contaminated by or a spurious detection of an image artifact |
smallint |
2 |
|
|
|
w4cc_map_str |
allwise_sc |
WISE |
Contamination and confusion string. This column is a character string that denotes all artifacts that may contaminate the W4 measurement of this source, in the priority order D,P,H,O,d,p,h,o. Lower-case letters denote cases where the source detection in this band is believed to be real but the measurement may be contaminated by the artifact. Upper-case letters denote cases where the source detection in this band may be a spurious detection of an artifact. This string is "null" if there are no artifacts that affect the measurement in this band. The value that appears in fourth element of the cc_flags string is the left-most character in w4cc_map_str. If w4cc_map_str is "null", then the corresponding cc_flags entry is "0". |
varchar |
9 |
|
|
|
For example, a real detection that is contaminated by a diffraction spike and a latent (persistent) image has a w?cc_map_str="dp". A spurious detection of a diffraction spike that is also contaminated by a latent image has w?cc_map_str="Dp". |
w4cc_map_str |
wise_allskysc |
WISE |
Contamination and confusion string in W4. This column is a character string that denotes all artifacts that may contaminate the W4 measurement of this source, in the priority order D,P,H,O |
char |
9 |
|
|
|
w4cc_map_str |
wise_prelimsc |
WISE |
Contamination and confusion string in W4 This column is a character string that denotes all artifacts that may contaminate the W4 measurement of this source, in the priority order D,P,H,O |
char |
9 |
|
|
|
w4conf |
allwise_sc |
WISE |
Estimated confusion noise in the W4 sky background annulus, in digital numbers. This number is the difference between the measured noise in the sky background w4sigsk and the noise measured in the same region on the Atlas Uncertainty Maps. |
float |
8 |
dn |
|
|
w4conf |
wise_allskysc, wise_prelimsc |
WISE |
Estimated confusion noise in the W4 sky background annulus, in digital numbers This number is the difference between the measured noise in the sky background w4sigsk and the noise measured in the same region on the Atlas Uncertainty Maps |
float |
8 |
ADU |
-0.9999995e9 |
|
w4cov |
allwise_sc |
WISE |
Mean pixel coverage in W4. This column gives the mean pixel value from the W4 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 16.5" centered on the position of this source. |
float |
8 |
|
|
|
W4cov may differ from the integer frame coverage value given in w4m for two reasons. First, individual pixels in the measurement area may be masked or otherwise unusable, reducing the effective pixel count and thus the mean coverage value. Second, the effective sky area sampled by a pixels in single-exposure image varies across the focal plane because of field distortion. Distortion is corrected when coadding to generate the Atlas Images. Therefore, the effective number of pixels contributing to a pixel in the Atlas Coverage Map may be slightly smaller or larger than expected if there was no distortion. |
w4cov |
wise_allskysc |
WISE |
Mean pixel coverage in W4. This column gives the mean pixel value from the W4 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 16.5" centered on the position of this source. |
real |
4 |
|
-0.9999995e9 |
|
w4cov |
wise_prelimsc |
WISE |
Mean pixel coverage in W4 This column gives the mean pixel value from the W4 Atlas Tile Coverage Map within the "standard" aperture, a circular area with a radius of 17.0" centered on the position of this source |
real |
4 |
|
-0.9999995e9 |
|
w4dmag |
wise_allskysc |
WISE |
Difference between maximum and minimum magnitude of the source from all usable single-exposure frames, W4. Single-exposure measurements with w4rchi2 values greater than 3.0 times the median are rejected from this computation. |
real |
4 |
mag |
-0.9999995e9 |
|
w4flg |
allwise_sc |
WISE |
W4 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg |
wise_allskysc |
WISE |
W4 "standard" aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
smallint |
2 |
|
-9999 |
|
w4flg |
wise_prelimsc |
WISE |
W4 "standard" aperture measurement quality flag This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit |
smallint |
2 |
|
-9999 |
|
w4flg_1 |
allwise_sc |
WISE |
W4 11.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_1 |
wise_allskysc |
WISE |
W4 11.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_1 |
wise_prelimsc |
WISE |
W4 11.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_2 |
allwise_sc |
WISE |
W4 16.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_2 |
wise_allskysc |
WISE |
W4 16.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_2 |
wise_prelimsc |
WISE |
W4 16.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_3 |
allwise_sc |
WISE |
W4 22.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_3 |
wise_allskysc |
WISE |
W4 22.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_3 |
wise_prelimsc |
WISE |
W4 22.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_4 |
allwise_sc |
WISE |
W4 27.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_4 |
wise_allskysc |
WISE |
W4 27.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_4 |
wise_prelimsc |
WISE |
W4 27.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_5 |
allwise_sc |
WISE |
W4 33.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_5 |
wise_allskysc |
WISE |
W4 33.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_5 |
wise_prelimsc |
WISE |
W4 33.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_6 |
allwise_sc |
WISE |
W4 38.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_6 |
wise_allskysc |
WISE |
W4 38.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_6 |
wise_prelimsc |
WISE |
W4 38.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_7 |
allwise_sc |
WISE |
W4 44.0" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_7 |
wise_allskysc |
WISE |
W4 44.0" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_7 |
wise_prelimsc |
WISE |
W4 44.0" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flg_8 |
allwise_sc |
WISE |
W4 49.5" radius aperture magnitude quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4flg_8 |
wise_allskysc |
WISE |
W4 49.5" radius aperture magnitude quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag. |
smallint |
2 |
|
-9999 |
|
w4flg_8 |
wise_prelimsc |
WISE |
W4 49.5" radius aperture magnitude quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the standard aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4flux |
allwise_sc |
WISE |
The "raw" W4 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w4flux |
wise_allskysc |
WISE |
The "raw" W4 source flux measured in profile-fit photometry in units of digital numbers. This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w4flux |
wise_prelimsc |
WISE |
The "raw" W4 source flux measured in profile-fit photometry in units of digital numbers This value may be negative. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w4frl |
wise_prelimsc |
WISE |
Fraction of W4 pixels affected by latents This column gives the fraction of all W4 pixels in the stack of individual W4 exposures used to characterize this source that may be affected by the presence of a latent image produced by a bright source |
real |
4 |
|
-0.9999995e9 |
|
w4frtr |
wise_allskysc |
WISE |
Fraction of W4 pixels affected by transients. This column gives the fraction of all W4 pixels in the stack of individual W4 exposures used to characterize this source that may be affected by transient events. This number is computed by counting the number of pixels in the single exposure Bit Mask images with value "21" that are present within the profile-fitting area, a circular region with radius of 15.0", centered on the position of this source, and dividing by the total number of pixels in the same area that are available for measurement. |
real |
4 |
|
-0.9999995e9 |
|
w4gerr |
allwise_sc |
WISE |
Uncertainty in the W4 magnitude of source measured in elliptical aperture. CAUTION: A w4gerr value of 9.999 indicates that the measurement uncertainty is very large, or the uncertainty could not be computed. In either case, the w4gmag measurement should be considered highly suspect. |
float |
8 |
mag |
|
|
w4gerr |
wise_allskysc |
WISE |
Uncertainty in the W4 magnitude of source measured in elliptical aperture. |
real |
4 |
mag |
-0.9999995e9 |
|
w4gerr |
wise_prelimsc |
WISE |
Uncertainty in the W4 magnitude of source measured in elliptical aperture |
real |
4 |
mag |
-0.9999995e9 |
|
w4gflg |
allwise_sc |
WISE |
W4 elliptical aperture measurement quality flag. This flag indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. |
int |
4 |
|
|
|
The flag value is an integer that is the combination of one or more of the following values that signify different conditions: - 0 - No contamination
- 1 - Source confusion - another source falls within the measurement aperture
- 2 - Presence of bad pixels in the measurement aperture
- 4 - Non-zero bit flag tripped (other than 2 or 18)
- 8 - All pixels are flagged as unusable, or the aperture flux is negative. In the former case, the aperture magnitude is "null". In the latter case, the aperture magnitude is a 95% confidence upper limit.
- 16 - Saturation - there are one or more saturated pixels in the measurement aperture
- 32 - The magnitude is a 95% confidence upper limit
|
w4gflg |
wise_allskysc |
WISE |
W4 elliptical aperture measurement quality flag. Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag, w4mflg. |
smallint |
2 |
|
-9999 |
|
w4gflg |
wise_prelimsc |
WISE |
W4 elliptical aperture measurement quality flag Indicates if one or more image pixels in the measurement aperture for this band is confused with nearby objects, is contaminated by saturated or otherwise unusable pixels, or is an upper limit. The flag values are as described for the "standard" aperture photometry quality flag |
smallint |
2 |
|
-9999 |
|
w4gmag |
allwise_sc |
WISE |
W4 magnitude of source measured in the elliptical aperture described by w4rsemi, w4ba, and w4pa. |
float |
8 |
mag |
|
|
w4gmag |
wise_allskysc |
WISE |
W4 magnitude of source measured in the elliptical aperture described by w4rsemi, w4ba, and w4pa. |
real |
4 |
mag |
-0.9999995e9 |
|
w4gmag |
wise_prelimsc |
WISE |
W4 magnitude of source measured in the elliptical aperture described by w4rsemi, w4ba, and w4pa |
real |
4 |
mag |
-0.9999995e9 |
|
w4k |
allwise_sc |
WISE |
Stetson K variability index (Stetson, P. 1996, PASP, 108, 851) computed using the W4 profile-fit fluxes measured on the individual single-exposure images. This column is null if there are <3 single-exposure measurements available in W4. |
float |
8 |
|
|
|
w4m |
allwise_sc |
WISE |
Integer frame coverage. This column gives the number of individual 8.8s W4 exposures on which a profile-fit measurement of this source was possible. This number can differ between the four bands because band-dependent criteria are used to select individual frames for inclusion in the coadded Atlas Images. This column is null if there is no frame coverage in this band at the position of this source. |
int |
4 |
|
|
|
w4m |
wise_allskysc |
WISE |
Integer frame coverage in W4. This column gives the number of individual 8.8s W4 exposures on which a profile-fit measurement of this source was possible. |
bigint |
8 |
|
-99999999 |
|
w4m |
wise_prelimsc |
WISE |
Integer frame coverage in W4 This column gives the number of individual 8.8s W4 exposures on which a profile-fit measurement of this source was possible |
bigint |
8 |
|
-99999999 |
|
w4mag |
allwise_sc |
WISE |
W4 "standard" aperture magnitude. This is the curve-of-growth corrected source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". The curve-of-growth correction is given in w4mcor. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag |
wise_allskysc, wise_prelimsc |
WISE |
W4 "standard" aperture magnitude This is the curve-of-growth corrected source brightness measured in an 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_1 |
allwise_sc |
WISE |
W4 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_1 |
wise_allskysc |
WISE |
W4 11.0" radius aperture magnitude. This is the calibrated source brightness measured in a 11.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_1 |
wise_prelimsc |
WISE |
W4 11.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_2 |
allwise_sc |
WISE |
W4 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_2 |
wise_allskysc |
WISE |
W4 16.5" radius aperture magnitude. This is the calibrated source brightness measured in a 16.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_2 |
wise_prelimsc |
WISE |
W4 16.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_3 |
allwise_sc |
WISE |
W4 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_3 |
wise_allskysc |
WISE |
W4 22.0" radius aperture magnitude. This is the calibrated source brightness measured in a 22.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_3 |
wise_prelimsc |
WISE |
W4 22.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_4 |
allwise_sc |
WISE |
W4 27.5" radius aperture magnitude. This is the calibrated source brightness measured in a 27.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied.This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_4 |
wise_allskysc |
WISE |
W4 27.5" radius aperture magnitude. This is the calibrated source brightness measured in a 27.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_4 |
wise_prelimsc |
WISE |
W4 27.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_5 |
allwise_sc |
WISE |
W4 33.0" radius aperture magnitude. This is the calibrated source brightness measured in a 33.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_5 |
wise_allskysc |
WISE |
W4 33.0" radius aperture magnitude. This is the calibrated source brightness measured in a 33.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_5 |
wise_prelimsc |
WISE |
W4 33.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_6 |
allwise_sc |
WISE |
W4 38.5" radius aperture magnitude. This is the calibrated source brightness measured in a 38.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_6 |
wise_allskysc |
WISE |
W4 38.5" radius aperture magnitude. This is the calibrated source brightness measured in a 38.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_6 |
wise_prelimsc |
WISE |
W4 38.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_7 |
allwise_sc |
WISE |
W4 44.0" radius aperture magnitude. This is the calibrated source brightness measured in a 44.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_7 |
wise_allskysc |
WISE |
W4 44.0" radius aperture magnitude. This is the calibrated source brightness measured in a 44.0" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_7 |
wise_prelimsc |
WISE |
W4 44.0" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_8 |
allwise_sc |
WISE |
W4 49.5" radius aperture magnitude. This is the calibrated source brightness measured in a 49.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is null if an aperture measurement was not possible in W4. |
float |
8 |
mag |
|
|
w4mag_8 |
wise_allskysc |
WISE |
W4 49.5" radius aperture magnitude. This is the calibrated source brightness measured in a 49.5" radius circular aperture centered on the source position on the Atlas Image. If the source is not detected in the aperture measurement, this is the 95% confidence upper limit to the brightness. The background sky reference level is measured in an annular region with inner radius of 50" and outer radius of 70". No curve-of-growth correction has been applied. This column is default if this aperture measurement was not possible in W4. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mag_8 |
wise_prelimsc |
WISE |
W4 49.5" radius aperture magnitude This column is default if this aperture measurement was not possible in W4 |
real |
4 |
mag |
-0.9999995e9 |
|
W4mag_ALLWISE |
ravedr5Source |
RAVE |
W4 magnitude from ALLWISE |
real |
4 |
mag |
|
phot.mag;em.opt |
w4magp |
allwise_sc |
WISE |
Magnitude computed from the inverse-variance-weighted mean of the profile-fit flux measurements on the w4m individual W4 frames covering this source. This differs from w4mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w4mpro is computed by fitting all W4 frames simultaneously and incorporating a robust error model. This column is "null" if w4m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w4mpro for the optimal flux measurement for point sources. |
float |
8 |
mag |
|
|
w4magp |
wise_allskysc |
WISE |
Inverse-variance-weighted mean W4 magnitude computed from profile-fit measurements on the w4m individual frames covering this source. This differs from w4mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w4mpro is computed by fitting all W4 frames simultaneously and incorporating a robust error model. This column is default if w4m=0, the mean flux is negative or if no individual frame measurements are possible. CAUTION: This is not a robust measurement of source brightness. It is provided as an internal repeatability diagnostic only. Users should always defer to w4mpro for the optimal flux measurement for point sources. |
real |
4 |
mag |
-0.9999995e9 |
|
w4magp |
wise_prelimsc |
WISE |
Inverse-variance-weighted mean W4 magnitude computed from profile-fit measurements on the w4m individual frames covering this source This differs from w4mpro in that it is computed by combining the profile-fit measurements from individual frames, whereas w4mpro is computed by fitting all W4 frames simultaneously and incorporating a robust error model. This column is default if w4m=0, the mean flux is negative or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mcor |
allwise_sc |
WISE |
W4 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 16.5" aperture photometry brightness, w4mag_2, to give the "standard-aperture" magnitude. |
float |
8 |
mag |
|
|
w4mcor |
wise_allskysc |
WISE |
W4 aperture curve-of-growth correction, in magnitudes. This correction is subtracted from the nominal 16.5" aperture photometry brightness, w4mag_2, to give the "standard-aperture" magnitude. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mcor |
wise_prelimsc |
WISE |
W4 aperture curve-of-growth correction, in magnitudes This correction is subtracted from the nominal 16.5" aperture photometry brightness, w4mag_2, to give the "standard-aperture" magnitude |
real |
4 |
mag |
-0.9999995e9 |
|
w4mjdmax |
allwise_sc, wise_allskysc |
WISE |
The latest modified Julian Date (mJD) of the W4 single-exposures covering the source. |
float |
8 |
|
|
|
w4mjdmean |
allwise_sc, wise_allskysc |
WISE |
The average modified Julian Date (mJD) of the W4 single-exposures covering the source. |
float |
8 |
|
|
|
w4mjdmin |
allwise_sc, wise_allskysc |
WISE |
The earliest modified Julian Date (mJD) of the W4 single-exposures covering the source. |
float |
8 |
|
|
|
w4mlq |
allwise_sc |
WISE |
Probability measure that the source is variable in W4 flux. The value is -ln(Q), where Q = 1 - P(χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
float |
8 |
|
|
|
The Q value is the fraction of all cases to be at least as large as that observed if the null hypothesis is true. The null hypothesis is that the flux is emitted by a non-variable astrophysical object. It may be false because the object is a true variable. It may also be false because the flux measurement is corrupted by artifacts such as cosmic rays, scattered light, etc. The smaller the Q value, the more implausible the null hypothesis, i.e., the more likely it is that the flux is either variable or corrupted or both. |
w4mlq |
wise_allskysc |
WISE |
Probability measure that the source is variable in W4 flux. The value is -log10(Q), where Q = 1 - P(Χ2). P is the cumulative chi-square distribution probability for the flux sample measured on the individual single-exposure images. The value is clipped at 9. |
int |
4 |
|
-99999999 |
|
w4mpro |
allwise_sc |
WISE |
W4 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W4 flux measurement has SNR<2. This column is null if the source is nominally detected in W4, but no useful brightness estimate could be made. |
float |
8 |
mag |
|
|
w4mpro |
wise_allskysc |
WISE |
W4 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W4 flux measurement has SNR<2. This column is default if the source is nominally detected in W4, but no useful brightness estimate could be made. |
real |
4 |
mag |
-0.9999995e9 |
|
w4mpro |
wise_prelimsc |
WISE |
W4 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W4 flux measurement has SNR<2 This column is default if the source is nominally detected in W4, but no useful brightness estimate could be made |
real |
4 |
mag |
-0.9999995e9 |
|
w4ndf |
allwise_sc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W4. |
int |
4 |
|
|
|
w4ndf |
wise_allskysc |
WISE |
Number of degrees of freedom in the flux variability chi-square, W4. |
bigint |
8 |
|
-99999999 |
|
w4nm |
allwise_sc |
WISE |
Integer frame detection count. This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W4 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
int |
4 |
|
|
|
w4nm |
wise_allskysc |
WISE |
Integer frame detection count in W4. This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W4 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures. |
bigint |
8 |
|
-99999999 |
|
w4nm |
wise_prelimsc |
WISE |
Integer frame detection count in W4 This column gives the number of individual 8.8s exposures on which this source was detected with SNR>3 in the W4 profile-fit measurement. This number can be zero for sources that are well-detected on the coadded Atlas Image, but too faint for detection on the single exposures |
bigint |
8 |
|
-99999999 |
|
w4pa |
allwise_sc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W4. |
float |
8 |
deg |
|
|
w4pa |
wise_allskysc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W4. |
real |
4 |
degrees |
-0.9999995e9 |
|
w4pa |
wise_prelimsc |
WISE |
Position angle (degrees E of N) of the elliptical aperture major axis used to measure source in W4 |
real |
4 |
degrees |
-0.9999995e9 |
|
w4rchi2 |
allwise_sc |
WISE |
Reduced χ2 of the W4 profile-fit photometry measurement. This column is null if the W4 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
|
|
w4rchi2 |
wise_allskysc |
WISE |
Reduced chi-squared of the W4 profile-fit photometry measurement. This column is default if the W4 magnitude is a 95% confidence upper limit (i.e. the source is not detected). |
real |
4 |
|
-0.9999995e9 |
|
w4rchi2 |
wise_prelimsc |
WISE |
Reduced chi-squared of the W4 profile-fit photometry measurement This column is default if the W4 magnitude is a 95% confidence upper limit (i.e. the source is not detected) |
real |
4 |
|
-0.9999995e9 |
|
w4rchi2_pm |
allwise_sc |
WISE |
Reduced χ2 of the W4 profile-fit photometry measurement including motion estimation. This column is null if the source is not detected in W4 or if the motion fit failed to converge or was not attempted. |
real |
4 |
|
|
|
w4rsemi |
allwise_sc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W4. |
float |
8 |
arcsec |
|
|
w4rsemi |
wise_allskysc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W4. |
real |
4 |
arcsec |
-0.9999995e9 |
|
w4rsemi |
wise_prelimsc |
WISE |
Semi-major axis of the elliptical aperture used to measure source in W4 |
real |
4 |
arcsec |
-0.9999995e9 |
|
w4sat |
allwise_sc |
WISE |
Saturated pixel fraction, W4. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W4]~0 mag. Saturation may occur in fainter sources because of charged particle strikes. |
float |
8 |
|
|
|
w4sat |
wise_allskysc |
WISE |
Saturated pixel fraction, W4. The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation. Saturation begins to occur for point sources brighter than [W4]~0 mag. Saturation may occur in fainter sources because of a charged particle strike. |
real |
4 |
|
-0.9999995e9 |
|
w4sat |
wise_prelimsc |
WISE |
Saturated pixel fraction, W4 The fraction of all pixels within the profile-fitting area in the stack of single-exposure images used to characterize this source that are flagged as saturated. A value larger than 0.0 indicates one or more pixels of saturation |
real |
4 |
|
-0.9999995e9 |
|
w4sigflux |
allwise_sc |
WISE |
Uncertainty in the "raw" W4 source flux measurement in profile-fit photometry in units of digital numbers. This column is null if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
dn |
|
|
w4sigflux |
wise_allskysc |
WISE |
Uncertainty in the "raw" W4 source flux measurement in profile-fit photometry in units of digital numbers. This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels. |
real |
4 |
ADU |
-0.9999995e9 |
|
w4sigflux |
wise_prelimsc |
WISE |
Uncertainty in the "raw" W4 source flux measurement in profile-fit photometry in units of digital numbers This column is default if no useful profile-fit measurement of the source is possible because of masked or otherwise unusable pixels |
real |
4 |
ADU |
-0.9999995e9 |
|
w4sigm |
allwise_sc |
WISE |
Uncertainty in the W4 "standard" aperture magnitude. This column is null if the W4 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm |
wise_allskysc, wise_prelimsc |
WISE |
Uncertainty in the W4 "standard" aperture magnitude This column is default if the W4 "standard" aperture magnitude is an upper limit, or if an aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_1 |
allwise_sc |
WISE |
Uncertainty in the W4 11.0" radius aperture magnitude. This column is null if the the 11.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_1 |
wise_allskysc |
WISE |
Uncertainty in the W4 11.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_1 |
wise_prelimsc |
WISE |
Uncertainty in the W4 11.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_2 |
allwise_sc |
WISE |
Uncertainty in the W4 16.5" radius aperture magnitude. This column is null if the the 16.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_2 |
wise_allskysc |
WISE |
Uncertainty in the W4 16.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_2 |
wise_prelimsc |
WISE |
Uncertainty in the W4 16.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_3 |
allwise_sc |
WISE |
Uncertainty in the W4 22.0" radius aperture magnitude. This column is null if the the 22.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_3 |
wise_allskysc |
WISE |
Uncertainty in the W4 22.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_3 |
wise_prelimsc |
WISE |
Uncertainty in the W4 22.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_4 |
allwise_sc |
WISE |
Uncertainty in the W4 27.5" radius aperture magnitude. This column is null if the the 27.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_4 |
wise_allskysc |
WISE |
Uncertainty in the W4 27.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_4 |
wise_prelimsc |
WISE |
Uncertainty in the W4 27.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_5 |
allwise_sc |
WISE |
Uncertainty in the W4 33.0" radius aperture magnitude. This column is null if the the 33.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_5 |
wise_allskysc |
WISE |
Uncertainty in the W4 33.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_5 |
wise_prelimsc |
WISE |
Uncertainty in the W4 33.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_6 |
allwise_sc |
WISE |
Uncertainty in the W4 38.5" radius aperture magnitude. This column is null if the the 38.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_6 |
wise_allskysc |
WISE |
Uncertainty in the W4 38.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_6 |
wise_prelimsc |
WISE |
Uncertainty in the W4 38.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_7 |
allwise_sc |
WISE |
Uncertainty in the W4 44.0" radius aperture magnitude. This column is null if the the 44.0" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_7 |
wise_allskysc |
WISE |
Uncertainty in the W4 44.0" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_7 |
wise_prelimsc |
WISE |
Uncertainty in the W4 44.0" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_8 |
allwise_sc |
WISE |
Uncertainty in the W4 49.5" radius aperture magnitude. This column is null if the the 49.5" radius aperture magnitude is an upper limit, or if an aperture measurement was not possible. |
float |
8 |
mag |
|
|
w4sigm_8 |
wise_allskysc |
WISE |
Uncertainty in the W4 49.5" radius aperture magnitude. This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigm_8 |
wise_prelimsc |
WISE |
Uncertainty in the W4 49.5" radius aperture magnitude This column is default if the corresponding aperture magnitude is an upper limit, or if that aperture measurement was not possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigmpro |
allwise_sc |
WISE |
W4 profile-fit photometric measurement uncertainty in mag units. This column is null if the W4 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
float |
8 |
mag |
|
|
w4sigmpro |
wise_allskysc |
WISE |
W4 profile-fit photometric measurement uncertainty. This column is default if the W4 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigmpro |
wise_prelimsc |
WISE |
W4 profile-fit photometric measurement uncertainty This column is default if the W4 profile-fit magnitude is a 95% confidence upper limit or if the source is not measurable |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigp1 |
allwise_sc |
WISE |
Standard deviation of the population of W4 fluxes measured on the w4m individual frames covering this source, in magnitudes. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is "null" if w4m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w4sigp1 |
wise_allskysc |
WISE |
Standard deviation of the population of W4 fluxes measured on the w4m individual frames covering this source. This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w4m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigp1 |
wise_prelimsc |
WISE |
Standard deviation of the population of W4 fluxes measured on the w4m individual frames covering this source This provides a measure of the characteristic uncertainty of the measurement of this source on individual frames. This column is default if w4m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigp2 |
allwise_sc |
WISE |
Standard deviation of the mean of the distribution of W4 fluxes (w4magp) computed from profile-fit measurements on the w4m individual frames covering this source, in magnitudes. This is equivalent to w4sigp1/sqrt(w4m). This column is "null" if w4m<2 or if no individual frame measurements are possible. |
float |
8 |
mag |
|
|
w4sigp2 |
wise_allskysc |
WISE |
Standard deviation of the mean of the distribution of W4 fluxes (w4magp) computed from profile-fit measurements on the w4m individual frames covering this source. This column is default if w4m<2 or if no individual frame measurements are possible. |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigp2 |
wise_prelimsc |
WISE |
Standard deviation of the mean of the distribution of W4 fluxes (w4magp) computed from profile-fit measurements on the w4m individual frames covering this source This column is default if w4m<2 or if no individual frame measurements are possible |
real |
4 |
mag |
-0.9999995e9 |
|
w4sigsk |
allwise_sc |
WISE |
The uncertainty in the W4 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". |
float |
8 |
dn |
|
|
w4sigsk |
wise_allskysc |
WISE |
The uncertainty in the W4 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" |
real |
4 |
ADU |
-0.9999995e9. |
|
w4sigsk |
wise_prelimsc |
WISE |
The uncertainty in the W4 sky background value in units of digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" |
real |
4 |
ADU |
-0.9999995e9 |
|
w4sky |
allwise_sc |
WISE |
The trimmed average of the W4 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
dn |
|
|
For profile-fit photometry, the sky background is measured on the individual single-exposure images that are used for source characterization. For aperture photometry, the sky background is measured on the Atlas Image. |
w4sky |
wise_allskysc |
WISE |
The trimmed average of the W4 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70". Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value. |
float |
8 |
ADU |
-0.9999995e9 |
|
w4sky |
wise_prelimsc |
WISE |
The trimmed average of the W4 sky background value in digital numbers measured in an annulus with an inner radius of 50" and outer radius of 70" Both profile-fit and aperture photometry source brightness measurements are made relative to this sky background value |
float |
8 |
ADU |
-0.9999995e9 |
|
w4snr |
allwise_sc |
WISE |
W4 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w4flux) to flux uncertainty (w4sigflux)in the W4 photometry measurement. This column is null if w4flux is negative, or if w4flux or w4sigflux are null. |
float |
8 |
|
|
|
w4snr |
wise_allskysc |
WISE |
W4 profile-fit measurement signal-to-noise ratio. This value is the ratio of the flux (w4flux) to flux uncertainty (w4sigflux)in the W4 profile-fit photometry measurement. This column is default if w4flux is negative, or if w4flux or w4sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
w4snr |
wise_prelimsc |
WISE |
W4 profile-fit measurement signal-to-noise ratio This value is the ratio of the flux (w4flux) to flux uncertainty (w4sigflux)in the W4 profile-fit photometry measurement. This column is default if w4flux is negative, or if w4flux or w4sigflux are default. |
real |
4 |
|
-0.9999995e9 |
|
W518F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 518/16 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W571F_D |
combo17CDFSSource |
COMBO17 |
flux in filter 571/25 in run D (07.10.-22.10.1999) |
float |
8 |
|
|
|
W571F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 571/25 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W571F_S |
combo17CDFSSource |
COMBO17 |
combined flux in filter 571/25; corrected for the gain of the CCD and only applied to objects without variability flag |
float |
8 |
|
|
|
W604F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 604/21 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W646F_D |
combo17CDFSSource |
COMBO17 |
flux in filter 646/27 in run D (07.10.-22.10.1999) |
float |
8 |
|
|
|
W696F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 696/20 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W753F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 753/18 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W815F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 815/20 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
W815F_G |
combo17CDFSSource |
COMBO17 |
flux in filter 815/20 in run G (19.01.-20.01.2001) |
float |
8 |
|
|
|
W815F_S |
combo17CDFSSource |
COMBO17 |
combined flux in filter 815/20; corrected for the gain of the CCD and only applied to objects without variability flag |
float |
8 |
|
|
|
W856F_D |
combo17CDFSSource |
COMBO17 |
flux in filter 856/14 in run D (07.10.-22.10.1999) |
float |
8 |
|
|
|
W914F_D |
combo17CDFSSource |
COMBO17 |
flux in filter 914/27 in run D (07.10.-22.10.1999) |
float |
8 |
|
|
|
W914F_E |
combo17CDFSSource |
COMBO17 |
flux in filter 914/27 in run E (28.01.-11.02.2000) |
float |
8 |
|
|
|
warnFlag |
firstSource |
FIRST |
Warning flag indicating that the source may be a sidelobe of a nearby bright source. |
varchar |
1 |
|
|
meta.code |
wcs |
RequiredDiffImage |
SHARKSv20210222 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
SHARKSv20210421 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
ULTRAVISTADR4 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR1 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR2 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR3 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR4 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR5 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSDR6 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20120926 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20130417 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20150108 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20160114 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20160507 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20170630 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20180419 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20201209 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20231101 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VHSv20240731 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEODR2 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEODR3 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEODR4 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEODR5 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEOv20100513 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIDEOv20111208 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGDR2 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGDR3 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGDR4 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20110714 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20111019 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20130417 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20150421 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20151230 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20160406 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20161202 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VIKINGv20170715 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDEEPv20230713 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDEEPv20240506 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDR1 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDR3 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDR4 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCDR5 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20110816 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20110909 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20120126 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20121128 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20130304 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20130805 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20140428 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20140903 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20150309 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20151218 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20160311 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20160822 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20170109 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20170411 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20171101 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20180702 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20181120 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20191212 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20210708 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20230816 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VMCv20240226 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVDR1 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVDR2 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVDR5 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVXDR1 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVv20100531 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcs |
RequiredDiffImage |
VVVv20110718 |
CASU difference image tool option to specify use of implicit WCS in the input files (y/n; recommended value=y) |
varchar |
1 |
|
|
?? |
wcsPass |
CurrentAstrometry |
SHARKSv20210222 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
SHARKSv20210421 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
ULTRAVISTADR4 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSDR1 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSDR2 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSDR3 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSDR4 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSDR5 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSDR6 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20120926 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSv20130417 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSv20140409 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSv20150108 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VHSv20160114 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20160507 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20170630 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20180419 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20201209 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20231101 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VHSv20240731 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VIDEODR2 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIDEODR3 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIDEODR4 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIDEODR5 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VIDEOv20100513 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIDEOv20111208 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGDR2 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGDR3 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGDR4 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGv20110714 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGv20111019 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGv20130417 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGv20140402 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VIKINGv20150421 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
|
wcsPass |
CurrentAstrometry |
VIKINGv20151230 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VIKINGv20160406 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VIKINGv20161202 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VIKINGv20170715 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCDEEPv20230713 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCDEEPv20240506 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCDR1 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCDR2 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCDR3 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCDR4 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCDR5 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20110816 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20110909 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20120126 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20121128 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20130304 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20130805 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20140428 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20140903 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20150309 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VMCv20151218 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20160311 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20160822 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20170109 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20170411 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20171101 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20180702 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20181120 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20191212 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20210708 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20230816 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VMCv20240226 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VVVDR1 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VVVDR2 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VVVDR5 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VVVXDR1 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs |
wcsPass |
CurrentAstrometry |
VVVv20100531 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
CurrentAstrometry |
VVVv20110718 |
Pass level of WCS {image extension keyword: WCSPASS} |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
wcsPass |
sharksCurrentAstrometry, ultravistaCurrentAstrometry, vhsCurrentAstrometry, videoCurrentAstrometry, vikingCurrentAstrometry, vmcCurrentAstrometry, vvvCurrentAstrometry |
VSAQC |
Pass level of WCS |
tinyint |
1 |
|
0 |
pos.wcs.cdmatrix |
weight |
ultravistaMapAverageWeights |
ULTRAVISTADR4 |
Normalised (conf=100 in a pawprint=1) weight of offset 1 |
real |
4 |
|
-9.999995e8 |
|
weighto1 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 1 |
real |
4 |
|
-9.999995e8 |
|
weighto1 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 1 |
real |
4 |
|
-9.999995e8 |
|
weighto2 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 2 |
real |
4 |
|
-9.999995e8 |
|
weighto2 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 2 |
real |
4 |
|
-9.999995e8 |
|
weighto3 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 3 |
real |
4 |
|
-9.999995e8 |
|
weighto3 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 3 |
real |
4 |
|
-9.999995e8 |
|
weighto4 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 4 |
real |
4 |
|
-9.999995e8 |
|
weighto4 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 4 |
real |
4 |
|
-9.999995e8 |
|
weighto5 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 5 |
real |
4 |
|
-9.999995e8 |
|
weighto5 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 5 |
real |
4 |
|
-9.999995e8 |
|
weighto6 |
vikingMapRemeasAver |
VIKINGZYSELJv20160909 |
Normalised (conf=100 in a pawprint=1) weight of offset 6 |
real |
4 |
|
-9.999995e8 |
|
weighto6 |
vikingMapRemeasAver |
VIKINGZYSELJv20170124 |
Normalised (conf=100 in a pawprint=1) weight of offset 6 |
real |
4 |
|
-9.999995e8 |
|
wfrtype |
Multiframe |
SHARKSv20210222 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
SHARKSv20210421 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
ULTRAVISTADR4 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR1 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR2 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR3 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR4 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR5 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSDR6 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20120926 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20130417 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20140409 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20150108 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20160114 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20160507 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20170630 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20180419 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20201209 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20231101 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VHSv20240731 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEODR2 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEODR3 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEODR4 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEODR5 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEOv20100513 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIDEOv20111208 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGDR2 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGDR3 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGDR4 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20110714 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20111019 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20130417 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20140402 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20150421 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20151230 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20160406 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20161202 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VIKINGv20170715 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDEEPv20230713 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDEEPv20240506 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDR1 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDR2 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDR3 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDR4 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCDR5 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20110816 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20110909 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20120126 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20121128 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20130304 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20130805 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20140428 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20140903 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20150309 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20151218 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20160311 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20160822 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20170109 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20170411 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20171101 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20180702 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20181120 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20191212 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20210708 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20230816 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VMCv20240226 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVDR1 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVDR2 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVDR5 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVXDR1 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVv20100531 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
Multiframe |
VVVv20110718 |
Mean sky frame {image primary HDU keyword: WFRTYPE} |
varchar |
4 |
|
NONE |
|
wfrtype |
sharksMultiframe, ultravistaMultiframe, vhsMultiframe, videoMultiframe, vikingMultiframe, vmcMultiframe, vvvMultiframe |
VSAQC |
Mean sky frame |
varchar |
4 |
|
NONE |
|
wise_avg_cont |
gaiaxwise_matches |
GAIAXWISE |
Mean contaminating relative flux within PSFs when constructing h_offsets for WISE sources at the local density, magnitude and intrinsic positional uncertainty of the primary source. |
float |
8 |
dimensionless |
|
|
wise_cntr |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
WISE integer unique source designation |
bigint |
8 |
dimensionless |
|
|
wise_cont_p1 |
gaiaxwise_matches |
GAIAXWISE |
Probability of WISE source having contaminant of at least 1% relative flux given its separation from its corresponding Gaia detection. |
float |
8 |
dimensionless |
|
|
wise_cont_p10 |
gaiaxwise_matches |
GAIAXWISE |
Probability of WISE source having contaminant of at least 10% relative flux given its separation from its corresponding Gaia detection. |
float |
8 |
dimensionless |
|
|
wise_dec |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
Celestial Declination |
float |
8 |
degrees |
|
pos.eq.dec;meta.main |
wise_designation |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
Sexagesimal, equatorial position-based source name in the form: hhmmss.ss+ddmmss.s. |
varchar |
32 |
dimensionless |
|
meta.id;meta.main |
wise_p |
wise_nonmatches |
GAIAXWISE |
match probability |
float |
8 |
dimensionless |
|
|
wise_ra |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
Celestial Right Ascension |
float |
8 |
degrees |
|
pos.eq.ra;meta.main |
wise_w1mpro |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
W1 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W1 flux measurement has SNR<2. |
float |
8 |
mag |
|
|
wise_w2mpro |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
W2 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W2 flux measurement has SNR<2. |
float |
8 |
mag |
|
|
wise_w3mpro |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
W3 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W3 flux measurement has SNR<2. |
float |
8 |
mag |
|
|
wise_w4mpro |
gaiaxwise_matches, wise_nonmatches |
GAIAXWISE |
W4 magnitude measured with profile-fitting photometry, or the magnitude of the 95% confidence brightness upper limit if the W4 flux measurement has SNR<2. |
float |
8 |
mag |
|
|
wiseID |
twompzPhotoz |
TWOMPZ |
WISE ID for wise_allskysc (cntr) |
bigint |
8 |
|
-99999999 |
meta.id |
wiseID |
wiseScosPhotoz, wiseScosPhotozRejects, wiseScosSvm |
WISExSCOSPZ |
WISE ID for the AllWISE source catalogue (allwise_sc.cntr) |
bigint |
8 |
|
-99999999 |
meta.id |
wiseX |
twompzPhotoz |
TWOMPZ |
WISE source designation in allskysc {image primary HDU keyword: WISE_designation} |
varchar |
22 |
|
NONE |
meta.id |
wiseX |
wiseScosPhotoz, wiseScosPhotozRejects |
WISExSCOSPZ |
WISE source designation in the AllWISE/ALLSKY source catalogue {image primary HDU keyword: designation} |
varchar |
22 |
|
NONE |
meta.id |
wiseX |
wiseScosSvm |
WISExSCOSPZ |
WISE source designation in the AllWISE/ALLSKY source catalogue {image primary HDU keyword: wise_designation} |
varchar |
22 |
|
NONE |
meta.id |
wx |
allwise_sc |
WISE |
The x-pixel coordinate of this source on the Atlas Image. |
float |
8 |
pix |
|
|
wx |
catwise_2020, catwise_prelim |
WISE |
x-pixel coordinate |
real |
4 |
pix |
|
|
wx |
wise_allskysc |
WISE |
The x-pixel coordinate of this source on the Atlas Image. |
real |
4 |
pixels |
|
|
wx |
wise_prelimsc |
WISE |
The x-pixel coordinate of this source on the Atlas Image |
real |
4 |
pixels |
|
|
wy |
allwise_sc |
WISE |
The y-pixel coordinate of this source on the Atlas Image. |
float |
8 |
pix |
|
|
wy |
catwise_2020, catwise_prelim |
WISE |
y-pixel coordinate |
real |
4 |
pix |
|
|
wy |
wise_allskysc |
WISE |
The y-pixel coordinate of this source on the Atlas Image. |
real |
4 |
pixels |
|
|
wy |
wise_prelimsc |
WISE |
The y-pixel coordinate of this source on the Atlas Image |
real |
4 |
pixels |
|
|