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 twotailed 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(1P(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 twotailed 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 twotailed 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 
crosscorrelation 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 (010) 
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 