gcns.rejectedivo://org.gavo.dc/gcns/q/rejectedThe GAVO DC teamSmart, R.L.Sarro, L.M.Rybizki, J.Reylé, C.Robin, A.C.Hambly, N.C.Abbas, U.Barstow, M.A.de Bruijne, J.H.J.Bucciarelli, B.Carrasco, J.M.Cooper, W.J.Hodgkin, S.T.Masana, E.Michalik, D.Sahlmann, J.Sozzetti, A.Gaia Collaboration2024-02-06T09:10:02ZGAVO Data Centre Team

Mönchhofstrasse 12-14, D-69120 Heidelberg

gavo@ari.uni-heidelberg.de+49 6221 54 1837catalogshertzsprung-russell-diagramluminosity-functionstellar-mass-functionssolar-neighborhoodThis is the catalogue of objects in the 8mas sample that were rejected for the main Gaia Catalogue of Nearby Stars as having a zero probability of being inside 100pc or indicated as a spurious astrometric solution.https://doi.org/10.1051/0004-6361/202039498http://dc.g-vo.org/tableinfo/gcns.rejectedCatalogResearchGaia0/0-11Opticalgcns This is a clean and well characterised catalogue of objects within 100pc of the Sun from the Gaia early third data release. We characterise the catalogue using the full data release, and comparisons to other catalogues in literature and simulations. For all candidates (measured parallax < 8 mas), we calculate a distance probability function using Bayesian procedures and mock catalogues for the prediction of the priors. For each entry using a random forest classifier we attempt to remove sources with spurious astrometric solutions. This results in 331312 objects that should contain at least 92% of stars within 100 pc at spectral type M9. GCNS comes with several auxiliary tables, in particular lists of resolved stellar systems, of known neary stars not found in eDR3 and of candidates of Hyades and ComaBer cluster members.gcns.rejectedThis is the catalogue of objects in the 8mas sample that were rejected for the main Gaia Catalogue of Nearby Stars as having a zero probability of being inside 100pc or indicated as a spurious astrometric solution.source_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainlongindexedprimaryraICRS right ascension from Gaia eDR3.degpos.eq.ra;meta.maindoubleindexednullabledecICRS declination from Gaia eDR3.degpos.eq.dec;meta.maindoubleindexednullablera_errorStandard error of ra (with cos δ applied).masstat.error;pos.eq.rafloatnullabledec_errorStandard error of decmasstat.error;pos.eq.decfloatnullableparallaxAbsolute barycentric stellar parallax of the source at the reference epoch J2016.0. If looking for a distance, consider joining with gedr3dist.main and using the distances from there.maspos.parallaxfloatnullableparallax_errorStandard error of parallaxmasstat.error;pos.parallaxfloatnullablepmraProper motion in right ascension of the source in ICRS at J2016.0. This is the tangent plane projection (i.e., multiplied by cos(δ)) of the proper motion vector in the direction of increasing right ascension.mas/yrpos.pm;pos.eq.rafloatnullablepmra_errorStandard error of pmramas/yrstat.error;pos.pm;pos.eq.rafloatnullablepmdecProper motion in declination at J2016.0.mas/yrpos.pm;pos.eq.decfloatnullablepmdec_errorStandard error of pmdecmas/yrstat.error;pos.pm;pos.eq.decfloatnullablephot_g_mean_magMean magnitude in the G band. This is computed from the G-band mean flux applying the magnitude zero-point in the Vega scale. To obtain error estimates, see phot_g_mean_flux_over_error.magphot.mag;em.opt;stat.meanfloatnullablephot_g_mean_flux_over_errorIntegrated mean G flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.stat.snr;phot.flux;em.opt;stat.meanfloatnullablephot_bp_mean_magMean magnitude in the integrated BP band. This is computed from the BP-band mean flux applying the magnitude zero-point in the Vega scale. To obtain error estimates, see phot_bp_mean_flux_over_error.magphot.mag;em.opt.Bfloatnullablephot_bp_mean_flux_over_errorIntegrated mean BP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.stat.snr;phot.flux;em.opt.Bfloatnullablephot_rp_mean_magMean magnitude in the integrated RP band. This is computed from the RP-band mean flux applying the magnitude zero-point in the Vega scale. To obtain error estimates, see phot_rp_mean_flux_over_error.magphot.mag;em.opt.Rfloatnullablephot_rp_mean_flux_over_errorIntegrated mean RP flux divided by its error. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.stat.snr;phot.flux;em.opt.Rfloatnullablephot_bp_rp_excess_factorBP/RP excess factor estimated from the comparison of the sum of integrated BP and RP fluxes with respect to the flux in the G band. This measures the excess of flux in the BP and RP integrated photometry with respect to the G band. This excess is believed to be caused by background and contamination issues affecting the BP and RP data. Therefore a large value of this factor for a given source indicates systematic errors in the BP and RP photometry.stat.fit.goodnessfloatnullableruweRenormalized Unit Weight Error; this is a revised measure for the overall consistency of the solution as defined by GAIA-C3-TN-LU-LL-124-01. A suggested cut on this is RUWE <1.40) See the note for details.stat.weightfloatnullableipd_frac_multi_peakPercentage of distance windows in which a double peak was seen (high values mean high likelihood of a resolved double star).meta.code.multipshortadoptedrvAdopted Radial Velocitykm/sphys.veloc;pos.heliocentricfloatnullableadoptedrv_errorError in adopted RVkm/sstat.error;phys.veloc;pos.heliocentricfloatnullableadoptedrv_refnameBibcode for the source of the radial velocitymeta.bib.bibcodecharnullableradial_velocity_is_valid1 if this object has a radial velocity in eDR3, 0 otherwisemeta.code.qualshortgcns_probProbability that the astrometry is reliablestat.fit.goodnessfloatnullablewd_probprobability that this is a white dwarf.stat.likelihood;src.classfloatnullabledist_11st percentile of the distance PDF, used in GCNS selectionkpcstat.value;pos.distancefloatnullabledist_1616th percentile of the distance PDF (1 σ lower bound)kpcstat.value;pos.distancefloatnullabledist_50Median of the distance PDFkpcpos.distance;stat.medianfloatnullabledist_8484th percentile of the distance PDF (1 σ upper bound)kpcstat.value;pos.distancefloatnullablexcoord_50Median x coordinate in the Galactic frame assuming dist_50pcpos.cartesian.x;stat.medianfloatnullablexcoord_161 σ lower bound of Galactic frame x coordinatepcstat.value;pos.cartesian.xfloatnullablexcoord_841 σ upper bound of Galactic frame x coordinatepcstat.value;pos.cartesian.xfloatnullableycoord_50Median y coordinate in the Galactic frame assuming dist_50pcpos.cartesian.y;stat.medianfloatnullableycoord_161 σ lower bound of Galactic frame y coordinatepcstat.value;pos.cartesian.yfloatnullableycoord_841 σ upper bound of Galactic frame y coordinatepcstat.value;pos.cartesian.yfloatnullablezcoord_50Median z coordinate in the Galactic frame assuming dist_50pcpos.cartesian.z;stat.medianfloatnullablezcoord_161 σ lower bound of Galactic frame z coordinatepcstat.value;pos.cartesian.zfloatnullablezcoord_841 σ upper bound of Galactic frame z coordinatepcstat.value;pos.cartesian.zfloatnullableuvel_50Median velocity u in the Galactic frame, direction positive xkm/sphys.veloc;pos.cartesian.x;stat.medianfloatnullableuvel_161 σ lower bound for ukm/sstat.value;phys.veloc;pos.cartesian.xfloatnullableuvel_841 σ upper bound for ukm/sstat.value;phys.veloc;pos.cartesian.xfloatnullablevvel_50Median velocity v in the Galactic frame, direction positive ykm/sphys.veloc;pos.cartesian.y;stat.medianfloatnullablevvel_161 σ lower bound for vkm/sstat.value;phys.veloc;pos.cartesian.yfloatnullablevvel_841 σ upper bound for vkm/sstat.value;phys.veloc;pos.cartesian.yfloatnullablewvel_50Median velocity w in the Galactic frame, direction positive zkm/sphys.veloc;pos.cartesian.z;stat.medianfloatnullablewvel_161 σ lower bound for wkm/sstat.value;phys.veloc;pos.cartesian.zfloatnullablewvel_841 σ upper bound for wkm/sstat.value;phys.veloc;pos.cartesian.zfloatnullablename_gunnObject Name from PanSTARRS/SDSS/SkyMapper surveymeta.id.crosscharnullablerefname_gunnReference for the source of the Gunn photometrymeta.bib.bibcodecharnullablegmag_gunnGunn G band magnitude (when from SDSS, g, when from Skymapper, g_psf)magphot.mag;em.opt.Vfloatnullablee_gmag_gunnUncertainty in G band magnitudemagstat.error;phot.mag;em.opt.Vfloatnullablermag_gunnGunn R band magnitude (when from SDSS, g, when from Skymapper, g_psf)magphot.mag;em.opt.Rfloatnullablee_rmag_gunnUncertainty in R band magnitudemagstat.error;phot.mag;em.opt.Rfloatnullableimag_gunnGunn I band magnitude (when from SDSS, g, when from Skymapper, g_psf)magphot.mag;em.opt.Ifloatnullablee_imag_gunnUncertainty in I band magnitudemagstat.error;phot.mag;em.opt.Ifloatnullablezmag_gunnGunn Z band magnitude (when from SDSS, g, when from Skymapper, g_psf)magphot.mag;em.opt.Ifloatnullablee_zmag_gunnUncertainty in Z band magnitudemagstat.error;phot.mag;em.opt.Ifloatnullablename_2massName of this object in 2MASSmeta.id.crosscharnullablej_m_2mass2MASS J band magnitudemagphot.mag;em.IR.Jfloatnullablej_msig_2massUncertainty in 2MASS J band magnitudemagstat.error;phot.mag;em.IR.Jfloatnullableh_m_2mass2MASS H band magnitudemagphot.mag;em.IR.Hfloatnullableh_msig_2massUncertainty in 2MASS H band magnitudemagstat.error;phot.mag;em.IR.Hfloatnullablek_m_2mass2MASS K band magnitudemagphot.mag;em.IR.Kfloatnullablek_msig_2massUncertainty in 2MASS K band magnitudemagstat.error;phot.mag;em.IR.Kfloatnullablename_wiseName of this object in WISEmeta.id.crosscharnullablew1mpro_pm_wiseCATWISE W1 band magnitudemagphot.mag;em.IR.3-4umfloatnullablew1sigmpro_pm_wiseUncertainty in CATWISE W1 band magnitudemagstat.error;phot.mag;em.IR.3-4umfloatnullablew2mpro_pm_wiseCATWISE W2 band magnitudemagphot.mag;em.IR.4-8umfloatnullablew2sigmpro_pm_wiseUncertainty in CATWISE W2 band magnitudemagstat.error;phot.mag;em.IR.4-8umfloatnullablew3mpro_wiseCATWISE W3 band magnitudemagphot.mag;em.IR.8-15umfloatnullablew3sigmpro_wiseUncertainty in CATWISE W3 band magnitudemagstat.error;phot.mag;em.IR.8-15umfloatnullablew4mpro_wiseALLWISE W4 band magnitudemagphot.mag;em.IR.15-30umfloatnullablew4sigmpro_wiseUncertainty in ALLWISE W4 band magnitudemagstat.error;phot.mag;em.IR.15-30umfloatnullable