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Start Over Subject milky-way-galaxy Content Level Research Instrument Gaia
1. Estimated distances to 1.33 billion stars in Gaia DR2
ID:
ivo://org.gavo.dc/gdr2dist/q/cone
Title:
Estimated distances to 1.33 billion stars in Gaia DR2
Short Name:
gdr2dist scs
Date:
04 Apr 2022 15:48:41
Publisher:
The GAVO DC team
Description:
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.html
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:
29 Aug 2022 10:46:03
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:
29 Aug 2022 10:46:03
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