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Table: des_dr1.sgsep_stripe82_tests_v2
(The bold columns are indexed columns)
Column NameDescriptionDatatype
adaboost_pgalThe star-galaxy classifier using a machine learning framework based on the scikit package, using the SExtractor outputs. Values closer to 1 correspond to galaxies, larger values correspond to starsDOUBLE
adaboost_pgal_mofThe star-galaxy classifier using a machine learning framework based on the scikit package, using the MOF outputs. Values closer to 1 correspond to galaxies, larger values correspond to starsDOUBLE
class_star_iSExtractors neural network star-galaxy classifier (Bertin & Arnouts 1998), measured on the i-band coadd image. 0 - extended. 1 - point sourceREAL
cm_tA size estimator from the MOF pipeline, this is the parameter in the Gaussian mixture model corresponding to the trace of the unweighted second moments matrixDOUBLE
cm_t_errError on CM_TDOUBLE
coadd_objects_idY1A1 unique object IDBIGINT
concentration_mof_gMAG_PSF_MOF_G - MAG_CM_MOF_GDOUBLE
concentration_mof_iMAG_PSF_MOF_I - MAG_CM_MOF_IDOUBLE
concentration_mof_rMAG_PSF_MOF_R - MAG_CM_MOF_RDOUBLE
concentration_mof_zMAG_PSF_MOF_z - MAG_CM_MOF_zDOUBLE
decObject DEC (J2000)DOUBLE
galsift_pgal_mofThe star-galaxy classifier using the machine learning method based on MultiClass (Soumagnac et al. 2015), using MOF outputs. Values closer to 1 correspond to galaxies, larger values correspond to starsDOUBLE
jmksextJ-K from VHS data (stripe 82 only)REAL
mag_auto_gMagnitude estimation in g, for an elliptical model based on the Kron radius [mag]REAL
mag_auto_iMagnitude estimation in i, for an elliptical model based on the Kron radius [mag]REAL
mag_auto_rMagnitude estimation in r, for an elliptical model based on the Kron radius [mag]REAL
mag_auto_yMagnitude estimation in Y, for an elliptical model based on the Kron radius [mag]REAL
mag_auto_zMagnitude estimation in z, for an elliptical model based on the Kron radius [mag]REAL
mag_cm_mof_gMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) from a Gaussian mixture model fit to the multiple epochs composing the detection. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in the above paper. [mag]REAL
mag_cm_mof_iMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) from a Gaussian mixture model fit to the multiple epochs composing the detection. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in the above paper. [mag]REAL
mag_cm_mof_rMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) from a Gaussian mixture model fit to the multiple epochs composing the detection. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in the above paper. [mag]REAL
mag_cm_mof_zMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) from a Gaussian mixture model fit to the multiple epochs composing the detection. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in the above paper. [mag]REAL
mag_psf_mof_gMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) using the flux through the PSF estimated model. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in Drlica Wagner et al. (2018) . [mag]DOUBLE
mag_psf_mof_iMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) using the flux through the PSF estimated model. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in Drlica Wagner et al. (2018) . [mag]DOUBLE
mag_psf_mof_rMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) using the flux through the PSF estimated model. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in Drlica Wagner et al. (2018) . [mag]DOUBLE
mag_psf_mof_zMagnitude estimation, using the MOF code (see https://ui.adsabs.harvard.edu/abs/2018ApJS..235...33D/abstract) using the flux through the PSF estimated model. This magnitude is corrected by stellar locus regression (including the effect of extinction using SFD98 maps) as explained in Drlica Wagner et al. (2018) . [mag]DOUBLE
magerr_auto_gUncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag]REAL
magerr_auto_iUncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag]REAL
magerr_auto_rUncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag]REAL
magerr_auto_yUncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag]REAL
magerr_auto_zUncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag]REAL
raObject RA (J2000)DOUBLE
spread_model_iMorphology based classifier based on comparison between a PSF versus exponential-PSF model. Values closer to 0 correspond to stars, larger values correspond to galaxiesREAL
spreaderr_model_iUncertainty in morphology based classifier based on comparison between PSF versus exponential-PSF modelREAL
true_classThe truth value for the object, according to the matched catalog. We assign 0 to galaxies and 1 to stars, according to the following criteria in the matched catalogs: *COSMOS: truth is given by MU_CLASS from Leauthaud et al. 2007 (1 - extended, 2 - point-like). *Hubble Source Catalog: truth is given from extendedness coefficient CI (CI < 1.2 for point-like objects). *VVDS: truth is given according to spectroscopic redshift (z < 0.001 for stars). *Stripe 82: truth is given according to spectroscopic redshift (z < 0.001 for stars).SMALLINT
zAvailable spectroscopic redshift for the objectDOUBLE