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Glossary of VSA attributes
This Glossary alphabetically lists all attributes used in the VSAv20241206 database(s) held in the VSA. If you would like to have more information about the schema tables please use the VSAv20241206 Schema Browser (other Browser versions).

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D

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Q

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W

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Q
Name	Schema Table	Database	Description	Type	Length	Unit	Default Value	Unified Content Descriptor
q12	allwise_sc	WISE	Correlation significance between W1 and W2. The value is -log10(Q2(rho12)), where Q2 is the two-tailed fraction of all cases expected to show at least this much apparent positive or negative correlation when in fact there is no correlation. The value is clipped at 9.	int	4
			When the number of measurements is large, the significance of correlation also tends to be large even though the correlations themselves may have a small magnitude. This is a typical manifestation of statistical significance increasing as the sample size increases; eventually the significant effect can be due to small correlated errors in background estimation or even roundoff errors. These effects tend to be small but become significant when there are enough observations of them. High flux correlation significance should be taken seriously only when the magnitude of the correlation is also fairly high.
q12	catwise_2020, catwise_prelim	WISE	-log10(1-P(rho12)) given no real correlation	int	4
q12	wise_allskysc	WISE	Correlation significance between W1 and W2.	int	4
q23	allwise_sc	WISE	Correlation significance between W2 and W3. The value is -log10(Q2(rho23)), where Q2 is the two-tailed fraction of all cases expected to show at least this much apparent positive or negative correlation when in fact there is no correlation. The value is clipped at 9.	int	4
			When the number of measurements is large, the significance of correlation also tends to be large even though the correlations themselves may have a small magnitude. This is a typical manifestation of statistical significance increasing as the sample size increases; eventually the significant effect can be due to small correlated errors in background estimation or even roundoff errors. These effects tend to be small but become significant when there are enough observations of them. High flux correlation significance should be taken seriously only when the magnitude of the correlation is also fairly high.
q23	wise_allskysc	WISE	Correlation significance between W2 and W3.	int	4
q34	allwise_sc	WISE	Correlation significance between W3 and W4. The value is -log10(Q2(rho34)), where Q2 is the two-tailed fraction of all cases expected to show at least this much apparent positive or negative correlation when in fact there is no correlation. The value is clipped at 9.	int	4
			When the number of measurements is large, the significance of correlation also tends to be large even though the correlations themselves may have a small magnitude. This is a typical manifestation of statistical significance increasing as the sample size increases; eventually the significant effect can be due to small correlated errors in background estimation or even roundoff errors. These effects tend to be small but become significant when there are enough observations of them. High flux correlation significance should be taken seriously only when the magnitude of the correlation is also fairly high.
q34	wise_allskysc	WISE	Correlation significance between W3 and W4.	int	4
q_de_m_deg	tycho2	GAIADR1	Goodness of fit for mean Dec	real	4			meat.code.qual
Q_FINAL	spectra	SIXDF	suggested quality for redshift	int	4
q_pm_de	tycho2	GAIADR1	Goodness of fit for pm_de	real	4			meat.code.qual
q_pm_ra	tycho2	GAIADR1	Goodness of fit for pm_ra	real	4			meat.code.qual
q_ra_m_deg	tycho2	GAIADR1	Goodness of fit for mean RA	real	4			meat.code.qual
Q_Z_ABS	spectra	SIXDF	cross-correlation quality	int	4
Q_Z_EMI	spectra	SIXDF	emission redshift quality	int	4
qFlag	mcps_lmcSource, mcps_smcSource	MCPS	Quality flag (unique sum of the following flags): 0 = no flag; 1 = star for which photometry was replaced with that from Massey's catalog (Massey P., 2001, ApJS, in press); 2 = star for which photometry was replaced with that from OGLE; 10 = star with a successful stellar atmosphere model (Χ²<3) fit; 20 = star with an unsuccessful stellar atmosphere model fit.	smallint	2
qual	twomass_scn	TWOMASS	Quality score for scan.	smallint	2			meta.code
qual	twomass_sixx2_scn	TWOMASS	quality score for scan (0-10)	smallint	2
Qual_I	denisDR3Source	DENIS	Quality flag for I band [0,100]	smallint	2
Qual_J	denisDR3Source	DENIS	Quality flag for J band [0,100]	smallint	2
Qual_K	denisDR3Source	DENIS	Quality flag for K band [0,100]	smallint	2
QUALITY	mgcBrightSpec	MGC	Quality class	tinyint	1
QUALITY	spectra	SIXDF	redshift measurement quality: 4=good 1=bad (6=star)	int	4
qualityFlag	ObjectThin	PS1DR2	Subset of objInfoFlag denoting whether this object is real or a likely false positive. Values listed in ObjectQualityFlags	tinyint	1		0	meta.code.qual