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Start Over Subject stellar-distance Capability Type Table Access Protocol
1. A classifier for spurious astrometric solutions in Gaia EDR3
ID:
ivo://org.gavo.dc/gedr3spur/q/main
Title:
A classifier for spurious astrometric solutions in Gaia EDR3
Short Name:
gedr3spur.main
Date:
27 Dec 2024 08:31:04
Publisher:
The GAVO DC team
Description:
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.
2. Gaia DR3 Lite Distances Subset Cone Search
ID:
ivo://org.gavo.dc/gedr3dist/q/cone
Title:
Gaia DR3 Lite Distances Subset Cone Search
Short Name:
DR3 lite+dist
Date:
27 Dec 2024 08:31:06
Publisher:
The GAVO DC team
Description:
This 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.
3. Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3 (eDR3)
ID:
ivo://org.gavo.dc/gedr3dist/q/main
Title:
Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3 (eDR3)
Short Name:
gedr3dist.main
Date:
27 Dec 2024 08:31:06
Publisher:
The GAVO DC team
Description:
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/form