gedr3spur.mainivo://org.gavo.dc/gedr3spur/q/mainThe GAVO DC teamRybizki, J.Green, G.M.Rix, H.-W.El-Badry, K.Demleitner, M.Zari, E.Udalski, A.Smart, R.LGould, A.2021-10-26T07:12:21Z2021-10-18GAVO Data Centre Team

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gavo@ari.uni-heidelberg.de+49 6221 54 1837stellar-distancetrigonometric-parallaxmeasurement-error-model This table contains estimates of the "fidelity" of Gaia eDR3 astrometric solutions, a measure of the likelihood the eDR3 solution is physical rather than spurious obtained using a neural network trained on a small, hand-selected sample.2022MNRAS.510.2597Rhttp://dc.g-vo.org/tableinfo/gedr3spur.mainCatalogResearchIsServedByGAVO Data Center TAP servicehttp://dc.g-vo.org/taphttps://dc.g-vo.org/tapGaiaNeural NetworkOpticalgedr3spur This table contains estimates of the "fidelity" of Gaia eDR3 astrometric solutions, a measure of the likelihood the eDR3 solution is physical rather than spurious obtained using a neural network trained on a small, hand-selected sample.gedr3spur.main This table contains estimates of the "fidelity" of Gaia eDR3 astrometric solutions, a measure of the likelihood the eDR3 solution is physical rather than spurious obtained using a neural network trained on a small, hand-selected sample.1500000000source_idGaia DR3 unique source identifier. Note that this *cannot* be matched against the DR1 or DR2 source_ids.meta.id;meta.mainlongindexedprimaryfidelity_v2A probability that eDR3 has a good astrometric solution for this source, with values between 0 (meaning likely spurious solution) and 1 (meaning likely good solution). This is the published probability estimate.stat.fitfloatindexednullabletheta_arcsec_worst_sourceDistance to the eDR3 source within 30 arcsec of the object for which ΔG-θ is maximal. See norm_dg for details.arcsecpos.angDistancefloatnullablenorm_dgThis is a heuristic measure for contamination by bright stars in the neighbourhood. It is computed as ΔG-θ, where θ is the distance to another Gaia eDR3 object in arcsec (reported in theta_arcsec_worst_source), and ΔG is the magnitude difference in mag. This column gives the maximum of the values for all eDR3 sources within 30 arcsecs of the object.instr.backgroundfloatnullabledist_nearest_neighbor_at_least_m2_brighterDistance to the nearest neighbour in gaia_source at least 2 m fainter than this source.arcsecpos.angDistancefloatnullabledist_nearest_neighbor_at_least_0_brighterDistance to the nearest neighbour in gaia_source at least as bright as this source.arcsecpos.angDistancefloatnullabledist_nearest_neighbor_at_least_2_brighterDistance to the nearest neighbour in gaia_source at least 2 m brighter than this source.arcsecpos.angDistancefloatnullabledist_nearest_neighbor_at_least_4_brighterDistance to the nearest neighbour in gaia_source at least 4 m brighter than this source.arcsecpos.angDistancefloatnullabledist_nearest_neighbor_at_least_6_brighterDistance to the nearest neighbour in gaia_source at least 6 m brighter than this source.arcsecpos.angDistancefloatnullabledist_nearest_neighbor_at_least_10_brighterDistance to the nearest neighbour in gaia_source at least 10 m brighter than this source.arcsecpos.angDistancefloatnullablefidelity_v1A probablity that eDR3 has a good astrometric solution for this source, with values between 0 (meaning likely spurious solution) and 1 (meaning likely good solution). This comes from a first version of the estimator that was reviewed based on an astro-ph paper.stat.fitfloatnullable