Gaia eDR3 source catalogue "light"ivo://org.gavo.dc/gaia/q3/edr3liteThe GAVO DC teamGAIA Collaboration2021-02-03T14:14:23ZGAVO Data Center TeamMönchhofstrasse 12-14, D-69120 Heidelberggavo@ari.uni-heidelberg.de++49 6221 54 1837starssurveysastrometryproper-motions This is a “light” version of the full Gaia eDR3 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 eDR3 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).http://dc.zah.uni-heidelberg.de/tableinfo/gaia.edr3liteserved-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 early Data Release 3 (eDR3)
This is gaia_source from the Gaia early Data Release 3, stripped to just
enough columns to enable basic science (but therefore a bit faster and
simpler to deal with than the full gaia_source table).
Note that on this server, there is also The gedr3dist.main, which gives
distances computed by Bailer-Jones et al. Use these in preference
to working with the raw parallaxes.
This server also carries the gedr3mock schema containing a simulation
of gaia_source based on a state-of-the-art galaxy model, computed
by Rybizki et al.gaia.edr3liteGaia eDR3 source catalogue "light" This is a “light” version of the full Gaia eDR3 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 eDR3 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).1811730688source_idGaia eDR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainlongindexedprimaryraBarycentric Right Ascension in ICRS at epoch J2016.0degpos.eq.ra;meta.maindoubleindexednullabledecBarycentric Declination in ICRS at epoch J2016.0degpos.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 J2016.0. This is the tangent plane projection of the proper motion vector in the direction of increasing right ascension.mas/yrpos.pm;pos.eq.rafloatindexednullablepmdecProper motion in declination at J2016.0.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 J2016.0. If looking for a distance, consider joining with gedr3dist.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. To obtain error estimates, see phot_g_mean_flux_over_error.magphot.mag;em.opt;stat.meanfloatindexednullablephot_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.s**-1stat.snr;phot.flux;em.opt;stat.meanfloatnullablephot_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_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.Rfloatindexednullablephot_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_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.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.goodnessfloatnullableastrometric_excess_noiseThis is the excess noise of the source, measuring the disagreement, expressed as an angle, between the observations of a source and the best-fitting standard astrometric model (using five astrometric parameters). A value of 0 signifies a well-behaved source, a positive value signifies that the residuals are larger than expected.masstat.fit.goodnessfloatnullabledr2_radial_velocitySpectroscopic radial velocity in the solar barycentric reference frame taken from DR2. The radial velocity provided is the median value of the radial velocity measurements at all epochs.km/sspect.dopplerVelocfloatnullabledr2_radial_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. Again, this is just taken over from DR2.km/sstat.error;spect.dopplerVelocfloatnullablepseudocolourEffective wavenumber of the source estimated in the final astrometric processing. The pseudocolour is the astrometrically estimated effective wavenumber of the photon flux distribution in the astrometric (G) band, estimated from the chromatic displacements of image centroids. The field is empty when chromaticity was instead taken into account using the photometrically determined ν_eff given in the field nu_eff_used_in_astrometry.um**-1em.wavenumber;phot.colorfloatnullablepseudocolour_errorStandard error of the pseudocolour.um**-1stat.error;em.wavenumber;phot.colorfloatnullablevisibility_periods_usedNumber of visibility periods (groups of observations at least 4 days apart) used in the astrometric solution. A small value (less than 10) indicates that the calculated parallax could be more vulnerable to error not reflected in the formal uncertainties.meta.number;obsshortastrometric_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.codeshortnullablerandom_indexRandom index that can be used to deterministically select subsetsmeta.codelongindexedruweRenormalized 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