DR3 lite+distivo://org.gavo.dc/gedr3dist/q/coneThe GAVO DC teamBailer-Jones, C.A.L.Rybizki, J.Fouesneau, M.Demleitner, M.Andrae, R.2022-08-26T08:08:44Z2022-08-29GAVO Data Centre Team

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gavo@ari.uni-heidelberg.de+49 6221 54 1837milky-way-galaxystellar-distancesurveysstarsThis service returns the most important Gaia DR3 gaia_source columns together with robust geometric and photogeometric distances for the ~1.47 billion objects in Bailer-Jones et al's distance catalogue.2021AJ....161..147Bhttp://dc.g-vo.org/gedr3dist/q/cone/infoCatalogResearchIsServedByGAVO Data Center TAP serviceThe Gaia eDR3 (photo-) geometric distances catalogue. is licensed under the `Creative Commons Attribution 4.0 License <http://creativecommons.org/licenses/by/4.0/>`_ .. image:: /static/img/ccby.png :alt: [CC-BY] http://dc.g-vo.org/gedr3dist/q/cone/formhttps://dc.g-vo.org/gedr3dist/q/cone/formhttp://dc.g-vo.org/gedr3dist/q/cone/scs.xml?https://dc.g-vo.org/gedr3dist/q/cone/scs.xml?GETapplication/x-votable+xmlRARight Ascension (ICRS decimal)degpos.eq.rarealDECDeclination (ICRS decimal)degpos.eq.decrealSRSearch radiusdegrealsource_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainintegerr_med_geoThe median of the geometric distance posterior. The geometric distance estimate.pcpos.distancerealr_med_photogeoThe median of the photogeometric distance posterior. The photogeometric distance estimate.pcpos.distancerealresponseformatFile 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.integer180100000true303.2851140.929480.001http://dc.g-vo.org/gedr3dist/q/cone/capabilitieshttps://dc.g-vo.org/gedr3dist/q/cone/capabilitieshttp://dc.g-vo.org/gedr3dist/q/cone/availabilityhttps://dc.g-vo.org/gedr3dist/q/cone/availabilityhttp://dc.g-vo.org/gedr3dist/q/cone/tableMetadatahttps://dc.g-vo.org/gedr3dist/q/cone/tableMetadatahttp://dc.g-vo.org/taphttps://dc.g-vo.org/tapGaia0/0-11http://dc.g-vo.org/gedr3dist/q/cone/coverageOpticalgedr3dist We estimate the distance from the Sun to sources in Gaia eDR3 that have parallaxes. We provide two types of distance estimate, together with their corresponding asymmetric uncertainties, using Bayesian posterior density functions that we sample for each source. Our prior is based on a detailed model of the 3D spatial, colour, and magnitude distribution of stars in our Galaxy that includes a 3D map of interstellar extinction. The first type of distance estimate is purely geometric, in that it only makes use of the Gaia parallax and parallax uncertainty. This uses a direction-dependent distance prior derived from our Galaxy model. The second type of distance estimate is photogeometric: in addition to parallax it also uses the source's G-band magnitude and BP-RP colour. This type of estimate uses the geometric prior together with a direction-dependent and colour-dependent prior on the absolute magnitude of the star. Our distance estimate and uncertainties are quantiles, so are invariant under logarithmic transformations. This means that our median estimate of the distance can be used to give the median estimate of the distance modulus, and likewise for the uncertainties. For applications that cannot be satisfied through TAP, you can download a `full table dump`_. .. _full table dump: /gedr3dist/q/download/formgedr3dist.litewithdistThis table joins the DR3 "lite" table (consisting only of the columns necessary for the most basic science) with the estimated geometric and photogeometric distances. Note that this is an inner join, i.e., DR3 objects without distance estimates will not show up here. Note: Due to current limitations of the postgres query planner, this table cannot usefully be used in positional joins ("crossmatches"). See the `Tricking the query planner`_ example. .. _tricking the query planner: http://dc.g-vo.org/tap/examples#Trickingthequeryplanner1470000000source_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainlongnullableraBarycentric 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 (i.e., multiplied by cos(δ)) 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.stat.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.goodnessfloatnullableradial_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.Ifloatnullableradial_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.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.weightfloatnullabler_med_geoThe median of the geometric distance posterior. The geometric distance estimate.pcpos.distancefloatindexednullabler_lo_geoThe 16th percentile of the geometric distance posterior. The lower 1-sigma-like bound on the confidence interval.pcpos.distance;stat.minfloatnullabler_hi_geoThe 84th percentile of the geometric distance posterior. The upper 1-sigma-like bound on the confidence interval.pcpos.distance;stat.maxfloatnullabler_med_photogeoThe median of the photogeometric distance posterior. The photogeometric distance estimate.pcpos.distancefloatindexednullabler_lo_photogeoThe 16th percentile of the photogeometric distance posterior. The lower 1-sigma-like bound on the confidence interval.pcpos.distance;stat.minfloatnullabler_hi_photogeoThe 84th percentile of the photogeometric distance posterior. The upper 1-sigma-like bound on the confidence interval.pcpos.distance;stat.maxfloatnullableflagAdditional information on the solution. Do not use for filtering (see table note in the reference URL).meta.codecharnullable