DR3 lite Coneivo://org.gavo.dc/gaia/q3/coneThe GAVO DC teamGAIA Collaboration2023-04-11T08:03:36Z2022-08-23GAVO Data Centre Team

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gavo@ari.uni-heidelberg.de+49 6221 54 1837starssurveysastrometryproper-motions This schema contains data re-published from the official Gaia mirrors (such as ivo://uni-heidelberg.de/gaia/tap) either to support combining its data with local tables (the various Xlite tables) or to make the data more accessible to VO clients (e.g., epoch fluxes). Other Gaia-related data is found in, among others, the gdr3mock, gdr3spec, gedr3auto, gedr3dist, gedr3mock, and gedr3spur schemas.https://dc.g-vo.org/gaia/q3/cone/infoIsServedByGAVO Data Center TAP serviceGAVO Data Center TAP service If you use public Gaia DR3 data in a paper, please take note of `ESAC's guide`_ on how to acknowledge and cite it. .. _ESAC's guide: https://gea.esac.esa.int/archive/documentation/GDR3/Miscellaneous/sec_credit_and_citation_instructions/http://dc.g-vo.org/gaia/q3/cone/scs.xml?https://dc.g-vo.org/gaia/q3/cone/scs.xml?GETapplication/x-votable+xmlRARight Ascension (ICRS decimal)degpos.eq.rarealDECDeclination (ICRS decimal)degpos.eq.decrealSRSearch radiusdegrealparallaxAbsolute 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.parallaxrealphot_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.meanrealphot_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.Brealphot_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.Rrealsource_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainintegerresponseformatFile format requested for output.meta.code.mimecharmaxrecMaximum number of records returned. Pass 0 to retrieve service parameters.integerverbExhaustiveness of column selection. VERB=1 only returns the most important columns, VERB=2 selects the columns deemed useful to the average user, VERB=3 returns a table with all available columns.integer180100000true303.2907413740.93029206114150040.001http://dc.g-vo.org/gaia/q3/cone/capabilitieshttps://dc.g-vo.org/gaia/q3/cone/capabilitieshttp://dc.g-vo.org/gaia/q3/cone/availabilityhttps://dc.g-vo.org/gaia/q3/cone/availabilityhttp://dc.g-vo.org/gaia/q3/cone/tableMetadatahttps://dc.g-vo.org/gaia/q3/cone/tableMetadatahttp://dc.g-vo.org/taphttps://dc.g-vo.org/tapGaia0/0-1157174 571741.986e-19 4.966e-19https://dc.g-vo.org/gaia/q3/cone/coverageOpticalgaia This schema contains data re-published from the official Gaia mirrors (such as ivo://uni-heidelberg.de/gaia/tap) either to support combining its data with local tables (the various Xlite tables) or to make the data more accessible to VO clients (e.g., epoch fluxes). Other Gaia-related data is found in, among others, the gdr3mock, gdr3spec, gedr3auto, gedr3dist, gedr3mock, and gedr3spur schemas.gaia.dr3lite This is gaia_source from the Gaia 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. The full DR3 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).1811709771source_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.main15118286476804.59792466834312e+174.280400489214347e+186.707472532802898e+1869175289932832044801.0longindexedprimaryraBarycentric Right Ascension in ICRS at epoch J2016.0degpos.eq.ra;meta.main1.63271e-0644.3559260.257327.9323601doubleindexednullabledecBarycentric Declination in ICRS at epoch J2016.0degpos.eq.dec;meta.main-89.8559-69.306-25.65858.828789.80891doubleindexednullablera_errorStandard error of ra (with cos δ applied).masstat.error;pos.eq.ra0.003892330.026180.36931612.747299.96761floatnullabledec_errorStandard error of decmasstat.error;pos.eq.dec0.004471330.0252670.34071910.084999.94791floatnullablepmraProper 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.ra-2290.75-10.761-2.510985.690194002.650.810079floatindexednullablepmdecProper motion in declination at J2016.0.mas/yrpos.pm;pos.eq.dec-5817.8-11.9807-3.107555.227451707.70.810079floatindexednullablepmra_errorStandard error of pmramas/yrstat.error;pos.pm;pos.eq.ra0.004197780.03003810.3524571.764463.427460.810079floatnullablepmdec_errorStandard error of pmdecmas/yrstat.error;pos.pm;pos.eq.dec0.005543070.02828050.3147091.553273.442090.810079floatnullableparallaxAbsolute 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.parallax-187.029-1.324720.3063952.29237269.0570.810079floatindexednullableparallax_errorStandard error of parallaxmasstat.error;pos.parallax0.007283380.0304280.3430891.506425.575540.810079floatnullablephot_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.mean1.7732815.506819.722921.033322.75070.996994floatindexednullablephot_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.mean1.0823740.8126240.3572759.6921526.20.996994floatnullablephot_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.R0.05457844.5115535.5538808.8234.28292e+070.85822floatnullablephot_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.R1.9687414.540418.604320.259924.64070.85822floatindexednullablephot_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.B0.05579282.6186215.1807468.8943.7971e+070.851071floatnullablephot_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.B2.39815.891120.294321.856525.31610.851071floatindexednullablephot_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.goodness0.05097181.059221.309752.559711726.670.850372floatnullableastrometric_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.goodness000.2528616.90813842.4691floatnullableradial_velocitySpectroscopic radial velocity in the solar barycentric reference frame. For stars brighter than about 12 mag, this is the median of all single-epoch measurements. For fainter stars, RV estimation is from a co-added spectrum.km/sspect.dopplerVeloc.opt;em.opt.I-861.114-102.485-3.6544796.6219859.690.0186703floatnullableradial_velocity_errorError in radial_velocity; this is the error of the median for bright stars. For faint stars, it is derived from the cross-correlation function.km/sstat.error;spect.dopplerVeloc0.1130010.2643623.2835211.2939.99630.0186703floatnullablepseudocolourEffective 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.color-2.223770.9691671.354041.720255.086220.486942floatnullablepseudocolour_errorStandard error of the pseudocolour.um**-1stat.error;em.wavenumber;phot.color0.001352550.02575120.1098140.3241780.9766360.486942floatnullablevisibility_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;obs15.016.028.0331.0shortastrometric_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.code33.031.095.0951.0shortnullablerandom_indexRandom index that can be used to deterministically select subsetsmeta.code054342273.3905836836.01757319938.899999918117097401.0longindexedruweRenormalized 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.weight0.2247530.9243341.022951.6219993.41370.810079floatnullable