Selections from Gaia Data Release 2 (DR2)ivo://org.gavo.dc/gaia/q2/dr2lightThe GAVO DC teamGAIA Collaboration2018-12-05GAVO Data Center TeamMönchhofstrasse 12-14, D-69120 Heidelberggavo@ari.uni-heidelberg.de++49 6221 54 1837AstrometryGaia This is a “light” version of the full Gaia DR2 gaia_source table,
containing the original astrometric and photmetric columns with just
enough additional information to let careful researchers notice when
data is becomes uncertain and the full error model should be
consulted. The full DR2 is available from numerous places in the VO
(in particular from the TAP services ivo://uni-heidelberg.de/gaia/tap
and ivo://esavo/gaia/tap).
This table also includes a column containing the Renormalized Unit
Weight Error RUWE (GAIA-C3-TN-LU-LL-124-01), a robust measure for the
consistency of the solution.
On this TAP service, there is the table gdr2dist.main containing
distances computed by Bailer-Jones et al
(:bibcode:`2018AJ....156...58B`). If in doubt, use these instead of
the parallaxes provided here.http://dc.zah.uni-heidelberg.de/tableinfo/gaia.dr2lightserved-byGAVO Data Center TAP servicehttp://dc.zah.uni-heidelberg.de/taphttps://dc.zah.uni-heidelberg.de/tapGaia0/0-1157174 571741.986e-19 4.966e-19OpticalgaiaSelections from Gaia Data Release 2 (DR2)
At the GAVO data Center, we hold several data collections part of
or derived from Gaia data release 2:
* A version of GDR2's gaia_source table with just enough columns
to allow basic science (but therefore a bit faster and simpler to
deal with than the full gaia_source table). This table also
has Lindegren's RUWE measure for filtering out marginal solutions.
* The light curves released with DR2 as both a TAP-queriable table
(light curves as arrays) and an SSA service.
* The gdr2dist.main table with distances estimates computed by
Bailer-Jones et al (:bibcode:`2018AJ....156...58B`) that should be
used in preference to simple parallax operations.
* The gdr2mock schema, which contains a virtual Gaia catalog
generated from a carefully built model of the Galaxy.gaia.dr2light This is a “light” version of the full Gaia DR2 gaia_source table,
containing the original astrometric and photmetric columns with just
enough additional information to let careful researchers notice when
data is becomes uncertain and the full error model should be
consulted. The full DR2 is available from numerous places in the VO
(in particular from the TAP services ivo://uni-heidelberg.de/gaia/tap
and ivo://esavo/gaia/tap).
This table also includes a column containing the Renormalized Unit
Weight Error RUWE (GAIA-C3-TN-LU-LL-124-01), a robust measure for the
consistency of the solution.
On this TAP service, there is the table gdr2dist.main containing
distances computed by Bailer-Jones et al
(:bibcode:`2018AJ....156...58B`). If in doubt, use these instead of
the parallaxes provided here.source_idUnique source identifier. Note that this *cannot* be matched against the DR1 source_id.meta.id;meta.mainlongindexedprimaryraBarycentric Right Ascension in ICRS at ref_epochdegpos.eq.ra;meta.maindoubleindexednullabledecBarycentric Declination in ICRS at ref_epochdegpos.eq.dec;meta.maindoubleindexednullablera_errorStandard error of ra (with cos δ applied).masstat.error;pos.eq.rafloatnullabledec_errorStandard error of decmasstat.error;pos.eq.decfloatnullablepmraProper motion in right ascension of the source in ICRS at ref_epoch. This is the projection of the proper motion vector in the direction of increasing right ascension.mas/yrpos.pm;pos.eq.rafloatindexednullablepmdecProper motion in declination at ref_epoch.mas/yrpos.pm;pos.eq.decfloatindexednullablepmra_errorStandard error of pmramas/yrstat.error;pos.pm;pos.eq.rafloatnullablepmdec_errorStandard error of pmdecmas/yrstat.error;pos.pm;pos.eq.decfloatnullableparallaxAbsolute barycentric stellar parallax of the source at the reference epoch ref_epoch. If looking for a distance, consider joining with gdr2dist.main and using the distances from there.maspos.parallaxfloatindexednullableparallax_errorStandard error of parallaxmasstat.error;pos.parallaxfloatnullablephot_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.magphot.mag;em.opt;stat.meanfloatindexednullablephot_g_mean_fluxG-band mean flux as electrons per second.s**-1phot.flux;em.opt;stat.meandoublenullablephot_g_mean_flux_errorError on phot_g_mean_fluxs**-1stat.error;phot.flux;em.opt;stat.meanfloatnullablephot_rp_mean_fluxMean flux in the integrated RP band.s**-1phot.flux;em.opt.Rdoublenullablephot_rp_mean_flux_errorError in the mean flux in the integrated RP band. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.s**-1stat.error;phot.flux;em.opt.Rfloatnullablephot_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. No error is provided for this quantity as the error distribution is only symmetric in flux space. For errors small compared to the flux (less than 10%, say), the magnitude error is well approximated by 1.09*flux/flux_err.magphot.mag;em.opt.Rfloatindexednullablephot_bp_mean_fluxMean flux in the integrated BP band.s**-1phot.flux;em.opt.Bdoublenullablephot_bp_mean_flux_errorError in the mean flux in the integrated BP band. Errors are computed from the dispersion about the weighted mean of the input calibrated photometry.s**-1stat.error;phot.flux;em.opt.Bfloatnullablephot_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. No error is provided for this quantity as the error distribution is only symmetric in flux space. For errors small compared to the flux (less than 10%, say), the magnitude error is well approximated by 1.09*flux/flux_err.magphot.mag;em.opt.Bfloatindexednullablephot_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.goodnessfloatnullableradial_velocitySpectroscopic radial velocity in the solar barycentric reference frame. The radial velocity provided is the median value of the radial velocity measurements at all epochs. Warning: in the vicinity of bright stars, DR2 RVs can be grossly wrong. See arXiv:1901.10460 for details.km/sspect.dopplerVelocfloatnullableradial_velocity_errorThe radial velocity error is the error on the median to which a constant noise floor of 0.11 km/s has been added in quadrature to take into account the calibration contribution.km/sstat.error;spect.dopplerVelocfloatnullableastrometric_gof_alGoodness-of-fit statistic of the astrometric solution for the source in the along-scan direction (you probably want to use RUWE instead of this).stat.fit.goodnessfloatnullableastrometric_params_solvedThis is a binary code indicating which astrometric parameters were estimated for the source. A set bit means the parameter was estimated. The least-significant bit represents α, the next bits δ, parallax, PM(RA) and PM(De). For Gaia DR2 the only relevant values are 31 (all five parameters solved) and 3 (only positions).meta.codefloatnullablerandom_indexRandom index that can be used to deterministically select subsetsmeta.codelongruweRenormalized 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.weightfloatnullable