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Table: des_dr1.sgsep_cosmos_tests_v2
(The bold columns are indexed columns)
| Column Name | Description | Datatype |
|---|---|---|
| class_star_i | SExtractors neural network star-galaxy classifier (Bertin & Arnouts 1998), measured on the i-band coadd image. 0 - extended. 1 - point source | REAL |
| cm_t | A size estimator from the MOF pipeline, this is the parameter in the Gaussian mixture model corresponding to the trace of the unweighted second moments matrix | DOUBLE |
| cm_t_err | Error on CM_T | DOUBLE |
| coadd_objects_id | Y1A1 unique object ID | BIGINT |
| concentration_mof_g | MAG_PSF_MOF_G - MAG_CM_MOF_G | DOUBLE |
| concentration_mof_i | MAG_PSF_MOF_I - MAG_CM_MOF_I | DOUBLE |
| concentration_mof_r | MAG_PSF_MOF_R - MAG_CM_MOF_R | DOUBLE |
| concentration_mof_z | MAG_PSF_MOF_R - MAG_CM_MOF_R | DOUBLE |
| dec | Object DEC (J2000) | DOUBLE |
| hb_prob | Probabilistic galaxy prediction using a template fitting code (Fadely et al. 2012, COSMOS only) | REAL |
| mag_auto_g | Magnitude estimation in g, for an elliptical model based on the Kron radius [mag] | REAL |
| mag_auto_i | Magnitude estimation in i, for an elliptical model based on the Kron radius [mag] | REAL |
| mag_auto_r | Magnitude estimation in r, for an elliptical model based on the Kron radius [mag] | REAL |
| mag_auto_y | Magnitude estimation in Y, for an elliptical model based on the Kron radius [mag] | REAL |
| mag_auto_z | Magnitude estimation in z, for an elliptical model based on the Kron radius [mag] | REAL |
| mag_cm_mof_g | Magnitude 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] | DOUBLE |
| mag_cm_mof_i | Magnitude 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] | DOUBLE |
| mag_cm_mof_r | Magnitude 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] | DOUBLE |
| mag_cm_mof_z | Magnitude 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] | DOUBLE |
| mag_psf_mof_g | Magnitude estimation, using the MOF code (see Drlica Wagner et al. (2018) ) 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_i | Magnitude estimation, using the MOF code (see Drlica Wagner et al. (2018) ) 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_r | Magnitude estimation, using the MOF code (see Drlica Wagner et al. (2018) ) 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_z | Magnitude estimation, using the MOF code (see Drlica Wagner et al. (2018) ) 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_g | Uncertainty in g magnitude estimation, for an elliptical model based on the Kron radius [mag] | REAL |
| magerr_auto_i | Uncertainty in i magnitude estimation, for an elliptical model based on the Kron radius [mag] | REAL |
| magerr_auto_r | Uncertainty in r magnitude estimation, for an elliptical model based on the Kron radius [mag] | REAL |
| magerr_auto_y | Uncertainty in Y magnitude estimation, for an elliptical model based on the Kron radius [mag] | REAL |
| magerr_auto_z | Uncertainty in z magnitude estimation, for an elliptical model based on the Kron radius [mag] | REAL |
| mcal_ratio | The size ratio between the model fit, using a single Gaussian, and a PSF fit, from the metacalibration pipeline (Sheldon & Huff 2017, Huff and Mandelbaum 2017) | DOUBLE |
| ra | Object RA (J2000) | DOUBLE |
| spread_model_i | Morphology based classifier based on comparison between a PSF versus exponential-PSF model. Values closer to 0 correspond to stars, larger values correspond to galaxies | REAL |
| spreaderr_model_i | Uncertainty in morphology based classifier based on comparison between PSF versus exponential-PSF model | REAL |
| true_class | The 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 |
