gdr2dist.distposivo://org.gavo.dc/gdr2dist/q/distposThe GAVO DC teamBailer-Jones, C.A.L.Rybizki, J.Fouesneau, M.Mantelet, G.Andrae, R.2022-04-04T15:48:41ZGAVO Data Centre Team

Mönchhofstrasse 12-14, D-69120 Heidelberg

gavo@ari.uni-heidelberg.de+49 6221 54 1837milky-way-galaxystellar-distancesurveysstars This catalogue provides distances estimates (and uncertainties therein) for 1.33 billion stars over the whole sky brighter than about G=20.7. These have been estimated using the parallaxes (and their uncertainties) from Gaia DR2. A Bayesian procedure was used involving a prior with a single parameter L(l,b), which varies smoothly with Galactic longitude and latitude according to a Galaxy model. The posterior is summarized with a point estimate (usually the mode) and a confidence interval (usually the 68% highest density interval). The estimation procedure is described in detail in the `accompanying paper`_, which also analyses the catalogue content. .. _accompanying paper: http://www.mpia.de/homes/calj/gdr2_distances.html2018AJ....156...58Bhttp://dc.g-vo.org/tableinfo/gdr2dist.distposCatalogResearchGaia0/0-11gdr2dist This catalogue provides distances estimates (and uncertainties therein) for 1.33 billion stars over the whole sky brighter than about G=20.7. These have been estimated using the parallaxes (and their uncertainties) from Gaia DR2. A Bayesian procedure was used involving a prior with a single parameter L(l,b), which varies smoothly with Galactic longitude and latitude according to a Galaxy model. The posterior is summarized with a point estimate (usually the mode) and a confidence interval (usually the 68% highest density interval). The estimation procedure is described in detail in the `accompanying paper`_, which also analyses the catalogue content. .. _accompanying paper: http://www.mpia.de/homes/calj/gdr2_distances.htmlgdr2dist.distpos This catalogue provides distances estimates (and uncertainties therein) for 1.33 billion stars over the whole sky brighter than about G=20.7. These have been estimated using the parallaxes (and their uncertainties) from Gaia DR2. A Bayesian procedure was used involving a prior with a single parameter L(l,b), which varies smoothly with Galactic longitude and latitude according to a Galaxy model. The posterior is summarized with a point estimate (usually the mode) and a confidence interval (usually the 68% highest density interval). The estimation procedure is described in detail in the `accompanying paper`_, which also analyses the catalogue content. .. _accompanying paper: http://www.mpia.de/homes/calj/gdr2_distances.htmlsource_idUnique source identifier. Note that this *cannot* be matched against the DR1 source_id.meta.id;meta.main208907211095044.314552101313878e+174.317781268923228e+186.712850540084986e+1869175102672243891201.0longnullabler_estEstimated distancepcpos.distance0.593017533.8972839.876067.725939.10.999997floatindexednullabler_loLower bound on the 1 σ confidence intervalpcpos.distance;stat.min0373.0561572.493977.791floatnullabler_hiUpper bound on the 1 σ confidence intervalpcpos.distance;stat.max0.59354750.5965190.929857.761floatnullabler_lenLength scale used in the prior for the distance estimation.pcstat.fit.param;pos.distance335.228465.4391472.562320.332597.671floatnullableresult_flagType of result.meta.code.qual01.01.01.021.0shortmodality_flagResult regime flag: number of modes in the posterior (1 or 2).meta.code11.01.01.021.0shortraBarycentric Right Ascension in ICRS at ref_epochdegpos.eq.ra;meta.maindoubleindexednullabledecBarycentric Declination in ICRS at ref_epochdegpos.eq.dec;meta.maindoubleindexednullable