arxiv: 2012.05220 · v2 · submitted 2020-12-09 · 🌌 astro-ph.SR · astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3

C. A. L. Bailer-Jones (1) , J. Rybizki (1) , M. Fouesneau (1) , M. Demleitner (2) , R. Andrae (1) ((1) Max Planck Institute for Astronomy , Heidelberg , (2) Astronomisches Rechen-Institut , Heidelberg)

Authors on Pith no claims yet

Pith reviewed 2026-05-15 04:28 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA

keywords Gaiaparallaxesstellar distancesMilky Wayphotogeometric distancescatalogueextinction

0 comments

The pith

A three-dimensional model of the Galaxy provides priors for estimating reliable distances to 1.47 billion stars from Gaia parallaxes.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The publication of billions of stellar parallaxes from Gaia offers a major advance, but many measurements are too uncertain for direct distance calculation. This work develops a probabilistic method that incorporates a prior based on a three-dimensional Galactic model, including extinction and survey limits. It produces both geometric distances using only parallax and direction, and photogeometric distances that additionally use color and magnitude information. These estimates come with asymmetric uncertainties and can be directly applied in distance modulus calculations. A catalogue covering nearly all Gaia stars is made available for public use.

Core claim

We infer two types of distance. The first, geometric, uses the parallax together with a direction-dependent prior on distance. The second, photogeometric, additionally uses the colour and apparent magnitude of a star, by exploiting the fact that stars of a given colour have a restricted range of probable absolute magnitudes (plus extinction). We provide a catalogue of 1.47 billion geometric and 1.35 billion photogeometric distances together with asymmetric uncertainty measures.

What carries the argument

A probabilistic distance estimation using a prior constructed from a three-dimensional model of the Galaxy that includes interstellar extinction and Gaia's magnitude limit.

If this is right

Photogeometric distances show higher accuracy and precision for stars with poor parallax measurements compared to geometric ones.
The distance estimates are quantiles of a posterior distribution and transform invariantly for use in the distance modulus formula.
Tests on simulated data and external validations confirm the reliability of the photogeometric estimates.
The full catalogue can be queried and cross-matched with the Gaia data using standard astronomical query languages.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

These distances could enable more accurate mapping of the Milky Way's structure and kinematics without relying on simple parallax inversion.
Future surveys with similar parallax data could adopt similar prior-based methods to improve distance estimates for distant stars.
Cross-matching this catalogue with other datasets may reveal new insights into stellar populations and extinction variations.

Load-bearing premise

The three-dimensional Galactic model accurately represents the true distribution of stars, extinction, and the survey selection function in all directions and magnitudes.

What would settle it

A comparison showing that the photogeometric distances deviate significantly from independent trigonometric or photometric distances for a large sample of well-measured stars would falsify the improvement claim.

read the original abstract

Stellar distances constitute a foundational pillar of astrophysics. The publication of 1.47 billion stellar parallaxes from Gaia is a major contribution to this. Yet despite Gaia's precision, the majority of these stars are so distant or faint that their fractional parallax uncertainties are large, thereby precluding a simple inversion of parallax to provide a distance. Here we take a probabilistic approach to estimating stellar distances that uses a prior constructed from a three-dimensional model of our Galaxy. This model includes interstellar extinction and Gaia's variable magnitude limit. We infer two types of distance. The first, geometric, uses the parallax together with a direction-dependent prior on distance. The second, photogeometric, additionally uses the colour and apparent magnitude of a star, by exploiting the fact that stars of a given colour have a restricted range of probable absolute magnitudes (plus extinction). Tests on simulated data and external validations show that the photogeometric estimates generally have higher accuracy and precision for stars with poor parallaxes. We provide a catalogue of 1.47 billion geometric and 1.35 billion photogeometric distances together with asymmetric uncertainty measures. Our estimates are quantiles of a posterior probability distribution, so they transform invariably and can therefore also be used directly in the distance modulus (5log10(r)-5). The catalogue may be downloaded or queried using ADQL at various sites (see http://www.mpia.de/homes/calj/gedr3_distances.html) where it can also be cross-matched with the Gaia catalogue.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

This paper ships a practical public catalogue of geometric and photogeometric distances for 1.47 billion Gaia EDR3 stars by scaling up an existing Bayesian method with a Galactic prior.

read the letter

The main thing to know is that Bailer-Jones and colleagues have produced and released distances for essentially the full EDR3 sample. Geometric distances use parallax plus a direction-dependent prior; photogeometric ones add colour and magnitude to tighten the posterior for stars with noisy parallaxes. The output is quantiles, which makes them easy to plug into distance modulus calculations without further adjustment. They report tests on simulated data and some external checks, and the photogeometric version shows better performance where parallaxes are poor. That is the concrete deliverable: a large, usable catalogue rather than a new theoretical framework. The method itself was laid out in earlier papers in the series, so this is mainly an application at scale plus the addition of the photogeometric variant. They incorporate extinction and the survey magnitude limit into the prior, which is sensible. The catalogue is already queryable via ADQL at several sites, which lowers the barrier for users. The soft spot is the Galactic model that supplies the prior. It is three-dimensional and direction-dependent, but its parameters come from fits whose details are not fully visible in the abstract, and any mismatch in the assumed stellar density, extinction map, or selection function will propagate into the distances, especially at large radii or in crowded fields. That is an inherent limitation of prior-based methods rather than a flaw in execution here. The paper is aimed at anyone who needs distances for large numbers of stars to study Milky Way structure, kinematics, or populations. It is not a methods breakthrough, but the scale and the public release make it worth referee time. I would send it to peer review; the community gains a concrete data product that can be checked against future releases or independent surveys.

Referee Report

0 major / 3 minor

Summary. The manuscript presents a probabilistic method to derive stellar distances from Gaia EDR3 parallaxes. Geometric distances combine the parallax with a direction-dependent prior from a three-dimensional Galactic model that incorporates extinction and the survey selection function. Photogeometric distances additionally use the star's colour and apparent magnitude to constrain the absolute magnitude. The authors release a public catalogue of 1.47 billion geometric and 1.35 billion photogeometric distance estimates, each given as quantiles of the posterior with asymmetric uncertainties, and demonstrate improved performance for poor-parallax stars via simulations and external validation.

Significance. If the central results hold, the catalogue constitutes a substantial community resource. It supplies ready-to-use distance estimates and uncertainties for the majority of Gaia stars where naive parallax inversion is unreliable, and the quantile representation permits direct propagation into distance-modulus calculations without additional bias. Public availability through ADQL queries and cross-matching with the Gaia catalogue maximises immediate scientific impact in Galactic structure, stellar populations, and exoplanet host characterisation.

minor comments (3)

Abstract: the statement that photogeometric estimates 'generally have higher accuracy and precision' would benefit from a quantitative summary (e.g., median fractional error reduction for ϖ/σ_ϖ < 5) so readers can immediately gauge the practical gain.
The description of the Galactic model prior (including how its parameters were fixed and how the extinction map and magnitude limit are implemented) should be expanded with explicit equations or a dedicated subsection to support full reproducibility.
Figure captions and table headers should explicitly state the percentile levels used for the reported asymmetric uncertainties (e.g., 16th–84th) and any flags for stars where the posterior is truncated by the prior.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive assessment of the manuscript, recognition of the catalogue as a community resource, and recommendation for minor revision. The report accurately summarizes our probabilistic approach to geometric and photogeometric distances using a three-dimensional Galactic prior that accounts for extinction and selection effects.

Circularity Check

0 steps flagged

No significant circularity; derivation uses independent external prior and external validation

full rationale

The paper's central derivation computes posterior quantiles for geometric distances (parallax likelihood times direction-dependent Galactic prior) and photogeometric distances (adding color-magnitude information). The prior is constructed from a pre-existing three-dimensional Galactic model that incorporates extinction and survey selection; this model is external to the present catalogue and not fitted within the paper's equations. The estimates are validated on simulated data and external benchmarks, with no step reducing by construction to a fitted input or self-citation chain. No self-definitional, fitted-input-called-prediction, or load-bearing self-citation patterns appear in the provided derivation chain.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The method rests on a pre-existing three-dimensional Galactic model whose parameters (stellar density laws, extinction map, magnitude limits) are treated as given; no new entities are postulated.

free parameters (1)

Galactic model parameters
The prior is constructed from a 3D model that includes fitted parameters for stellar distribution, extinction, and survey selection; these are not re-derived in the paper.

axioms (1)

domain assumption A direction-dependent prior on distance can be constructed from a three-dimensional model of the Galaxy that incorporates interstellar extinction and Gaia's variable magnitude limit.
Invoked to define the posterior for each star's distance.

pith-pipeline@v0.9.0 · 5645 in / 1307 out tokens · 47867 ms · 2026-05-15T04:28:39.910841+00:00 · methodology

discussion (0)

Forward citations

Cited by 21 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

VLTI/PIONIER imaging of post-AGB binaries. An INSPIRING hunt for inner rim substructures in circumbinary discs
astro-ph.SR 2026-05 unverdicted novelty 7.0

High-resolution interferometric imaging of eight post-AGB circumbinary discs reveals diverse inner-rim substructures including azimuthal brightness enhancements and arc-like features not explained by inclination alone.
ATOMIUM: Inner circumstellar envelopes of oxygen-rich AGB stars as revealed by highly excited SiO lines
astro-ph.SR 2026-05 unverdicted novelty 7.0

ALMA Band 6 data detect SiO emission and masers up to v=8 in AGB stars, showing clumpy distributions, velocity gradients, and a tentative link between emission radius and mass-loss rate.
AGILE detection of transient {\gamma}-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255
astro-ph.HE 2026-05 unverdicted novelty 7.0

AGILE archival data reveal gamma-ray flares from a source matching IGR J17354-3255, with orbital phase correlation supporting physical association and high-energy emission from SFXTs.
An Old, Low-mass, Metal-poor Hypervelocity Star Candidate Consistent with a Galactic Center Origin
astro-ph.GA 2026-04 unverdicted novelty 7.0

Discovery of the first old low-mass metal-poor hypervelocity star candidate consistent with ejection from the Galactic center via the Hills mechanism.
An Old, Low-mass, Metal-poor Hypervelocity Star Candidate Consistent with a Galactic Center Origin
astro-ph.GA 2026-04 unverdicted novelty 7.0

DESI-HVS1 is the first reported old, low-mass, metal-poor hypervelocity star candidate whose reconstructed orbit points to a Galactic Center origin.
White dwarf + M dwarf Detached Binaries in Long Period Radio Transients: Observed Binary Parameters, Evolution, and Population Constraints
astro-ph.SR 2026-04 unverdicted novelty 7.0

Two long period radio transients are detached white dwarf-M dwarf binaries with matching periods, massive cool crystallized white dwarfs, low inclinations, and an estimated population of 100-2000 such systems within 2 kpc.
TESS light curves of two new magnetic cataclysmic variables: an asynchronous polar at the period minimum, and an eclipsing system with a large spin-to-orbit ratio
astro-ph.SR 2026-03 unverdicted novelty 7.0

Two new short-period asynchronous magnetic cataclysmic variables were found, one candidate at the period minimum with spin-to-orbit ratio 0.9879 and an eclipsing system with ratio 0.867, supporting magnetic synchroniz...
The Distribution of Blue Straggler Stars in the Color-Magnitude Diagrams of Old Open Clusters
astro-ph.SR 2026-05 unverdicted novelty 6.0

Blue straggler stars in old open clusters predominantly appear near the terminal-age main sequence because mass transfer from asymptotic giant branch donors enriches their cores with helium.
Milky Way Dynamics Favor Dark Matter over Modified Gravity Models
astro-ph.GA 2026-05 unverdicted novelty 6.0

Milky Way radial and vertical dynamics are inconsistent with MOND and STVG but consistent with dark matter halos, disfavoring the former at high significance.
Tracing the kinematic perturbations of the Milky Way spiral arms with APOGEE DR17 and Gaia DR3
astro-ph.GA 2026-05 unverdicted novelty 6.0

A revised steady-state radial-velocity response model with both V_R,sin and V_R,cos terms constrains the Milky Way's two-armed spiral to a pitch angle of ~10° and local density contrast of 5-18% at the solar radius.
Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)
astro-ph.SR 2026-05 conditional novelty 5.0

Abundances and Ba isotopic ratios in TYC 6044-714-1 are best reproduced by s+r nucleosynthesis models; i+s+r models require extreme conditions and fail to match the full pattern.
Isolating Broadband Radio Technosignatures (BRaTs): A Framework for Detecting Planetary-Scale Leakage
astro-ph.IM 2026-05 unverdicted novelty 5.0

A tiered observational strategy is outlined to identify planetary-scale broadband radio technosignatures (BRaTs) from advanced civilizations up to 100 pc away using multi-parameter diagnostics to separate them from na...
Multi-wavelength outburst activity from EP J174942.2-384834: a very faint X-ray transient discovered by Einstein Probe
astro-ph.HE 2026-05 accept novelty 5.0

EP J174942.2-384834 is classified as a very faint X-ray transient black hole candidate based on its hard X-ray spectra, optical/UV brightening correlated with X-rays, and lack of radio emission.
Filter Design for Estimating the Stellar Metallicity of Metal-poor Stars from Gaia XP Spectra
astro-ph.SR 2026-04 unverdicted novelty 5.0

Optimized filters centered at 3920-3960 Angstrom yield metallicity estimates with 0.18-0.39 dex precision down to [Fe/H] ~ -4 for metal-poor stars from Gaia XP spectra, enabling a catalog of 14.5 million such stars.
Shortest period for outer orbit in compact hierarchical triple? Discovery of SB1 around V0885 Per
astro-ph.SR 2026-04 unverdicted novelty 5.0

Tentative detection of a 21.8-day SB1 around V0885 Per that could set a new record for the shortest outer orbit in a compact hierarchical triple, but poor spectra quality prevents confirmation of physical association.
The Metallicity Gradient of Sagittarius Dwarf Spheroidal Galaxy Prior to Infall Constrained by S-PLUS Observations of its Tidal Stream
astro-ph.GA 2026-04 conditional novelty 5.0

The Sagittarius dwarf progenitor had a metallicity gradient of roughly -0.3 dex per kpc prior to infall.
An Outer Giant Planet or Brown Dwarf in the 51 Pegasi System?
astro-ph.EP 2026-05 unverdicted novelty 4.0

Tentative evidence for a super-Jupiter at 15-100 AU or brown dwarf at 20-170 AU in 51 Pegasi from RV curvature, but the signal is likely driven by Lick/Hamilton instrument drift.
HD3191, the high-mass X-ray binary that wasn't there
astro-ph.HE 2026-05 conditional novelty 4.0

HD3191 is a single rapidly rotating B1 IV:nn star showing multi-mode non-radial pulsations, not a high-mass X-ray binary.
TOI-159 b: an eccentric hot-Jupiter planet around a young, pulsating $\gamma$ Doradus star
astro-ph.EP 2026-05 accept novelty 4.0

TOI-159 b is confirmed as the hottest known eccentric hot Jupiter (e = 0.24) with a 13-sigma Keplerian detection around a young gamma Doradus star, including a preliminary low-resolution transmission spectrum.
TESS Asteroseismology of Red Giants in the Old Metal-Rich Open Clusters NGC 188 & NGC 6791
astro-ph.SR 2026-04 unverdicted novelty 4.0

TESS asteroseismology of red giants in NGC 188 and NGC 6791 recovers masses around 1.1 solar masses, an RGB mass loss of 0.02 solar masses, and a 7 Gyr cluster age consistent with prior estimates.
An astrometric search for planets in debris disk systems
astro-ph.EP 2026-04 unverdicted novelty 4.0

Gaia astrometric quality metrics and a machine-learning classifier trained on known exoplanet hosts identify candidate stars with debris disks likely to host undetected planets.

Reference graph

Works this paper leans on

80 extracted references · 80 canonical work pages · cited by 20 Pith papers · 5 internal anchors

[1]

Pre-launch description

The Gaia astrophysical parameters inference system (Apsis). Pre-launch description. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201322344 , adsurl =

work page doi:10.1051/0004-6361/201322344
[2]

and Wilkinson, M

Finding rare objects and building pure samples: probabilistic quasar classification from low-resolution Gaia spectra. , keywords =. doi:10.1111/j.1365-2966.2008.13983.x , adsurl =

work page doi:10.1111/j.1365-2966.2008.13983.x 2008
[3]

F., Capozziello, S., & Dainotti, M

The ILIUM forward modelling algorithm for multivariate parameter estimation and its application to derive stellar parameters from Gaia spectrophotometry. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2009.16125.x , adsurl =

work page doi:10.1111/j.1365-2966.2009.16125.x 2009
[4]

2010, Monthly Notices of the Royal Astronomical Society, 408, 1181, doi: 10.1111/j.1365-2966.2010.17197.x

Bayesian inference of stellar parameters and interstellar extinction using parallaxes and multiband photometry. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2010.17699.x , adsurl =

work page doi:10.1111/j.1365-2966.2010.17699.x 2010
[5]

Overview of models, algorithms, and software implementation

The astrometric core solution for the Gaia mission. Overview of models, algorithms, and software implementation. , keywords =

work page
[6]

Gaia Early Data Release 3: Summary of the contents and survey properties

work page
[8]

Gaia Early Data Release 3: Parallax bias versus magnitude, colour, and position

work page
[9]

Gaia Early Data Release 3: Photometric content and validation

work page
[11]

Gaia Early Data Release 3: The Gaia Catalogue of Nearby Stars

work page
[16]

Pre-processing and source list creation

Gaia Data Release 1. Pre-processing and source list creation. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201628643 , adsurl =

work page doi:10.1051/0004-6361/201628643
[17]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The astrometric solution. , archivePrefix = "arXiv", eprint =

work page
[18]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Variability Processing and Analysis Results. , archivePrefix = "arXiv", eprint =

work page
[19]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The ground-based list of radial velocity standard stars. , archivePrefix = "arXiv", eprint =

work page
[20]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Processing, validation, and performance of the spectroscopic data. , archivePrefix = "arXiv", eprint =

work page
[21]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The Radial Velocity Spectrometer instrument. , archivePrefix = "arXiv", eprint =

work page
[22]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Cross match of Gaia observations. , archivePrefix = "arXiv", eprint =

work page
[23]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Processing of the Photometric Data. , archivePrefix = "arXiv", eprint =

work page
[24]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Apsis First astrophysical parameters. , archivePrefix = "arXiv", eprint =

work page
[25]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The archive visualisation service. , archivePrefix = "arXiv", eprint =

work page
[26]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Cross-match with external catalogues: algorithm and statistics. , archivePrefix = "arXiv", eprint =

work page
[27]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Validation of photometric data. , archivePrefix = "arXiv", eprint =

work page
[29]

, archivePrefix = "arXiv", eprint =

Distances from parallaxes: on the proper use of astrometric data. , archivePrefix = "arXiv", eprint =

work page
[30]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Variable stars in the colour-magnitude diagram. , archivePrefix = "arXiv", eprint =

work page
[31]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Parallaxes and proper motions of Milky Way satellites. , archivePrefix = "arXiv", eprint =

work page
[32]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Mapping the Milky Way kinematic and large scale structure. , archivePrefix = "arXiv", eprint =

work page
[33]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Asteroid astrometry. , archivePrefix = "arXiv", eprint =

work page
[34]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The Hertzsprung-Russell diagram. , archivePrefix = "arXiv", eprint =

work page
[35]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: The reference frame and fundamental physics from QSO astrometry. , archivePrefix = "arXiv", eprint =

work page
[36]

, archivePrefix = "arXiv", eprint =

Gaia Data Release 2: Calibration and mitigation of electronic offset effects. , archivePrefix = "arXiv", eprint =

work page
[37]

gdr2\_completeness: GaiaDR2 data retrieval and manipulation

work page
[38]

Astronomical Data Analysis Software and Systems XIV , year = 2005, series =

TOPCAT STIL: Starlink Table/VOTable Processing Software. Astronomical Data Analysis Software and Systems XIV , year = 2005, series =

work page 2005
[39]

Hunter, J. D. , Title =. Computing In Science & Engineering , Volume =

work page
[48]

Estimating Distances from Parallaxes. III. Distances of Two Million Stars in the Gaia DR1 Catalogue. , archivePrefix = "arXiv", eprint =

work page
[50]

Practical Bayesian Inference , publisher =

Practical Bayesian Inference. Practical Bayesian Inference , publisher =

work page
[62]

arXiv e-prints , keywords =

Kalkayotl: A cluster distance inference code. arXiv e-prints , keywords =

work page
[63]

ArXiv e-prints , keywords =

Improved distances to stars common to TGAS and RAVE. ArXiv e-prints , keywords =

work page
[64]

, keywords =

StarHorse: a Bayesian tool for determining stellar masses, ages, distances, and extinctions for field stars. , keywords =. doi:10.1093/mnras/sty330 , adsurl =

work page doi:10.1093/mnras/sty330
[65]

ArXiv e-prints , keywords =

Characterising Open Clusters in the solar neighbourhood with the Tycho- Gaia Astrometric Solution. ArXiv e-prints , keywords =

work page
[66]

, keywords =

Fundamental stellar parameters and metallicities from Bayesian spectroscopy: application to low- and high-resolution spectra. , keywords =. doi:10.1093/mnras/stu1072 , adsurl =

work page doi:10.1093/mnras/stu1072
[67]

Hierarchical probabilistic inference of the color-magnitude diagram and shrinkage of stellar distance uncertainties

Hierarchical Probabilistic Inference of the Color-Magnitude Diagram and Shrinkage of Stellar Distance Uncertainties. , keywords =. doi:10.3847/1538-3881/aa91d5 , archivePrefix =. 1703.08112 , adsurl =

work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aa91d5
[68]

ArXiv e-prints , keywords =

Improving \ Gaia \ parallax precision with a data-driven model of stars. ArXiv e-prints , keywords =

work page
[69]

Absolute Ages and Distances of 22 GCs using Monte Carlo Main-Sequence Fitting

Absolute Ages and Distances of 22 GCs Using Monte Carlo Main-sequence Fitting. , keywords =. doi:10.3847/1538-4357/aa6574 , archivePrefix =. 1703.01915 , adsurl =

work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa6574
[72]

2019, , 628, A94, 10.1051/0004-6361/201935765

Anders , F., Khalatyan , A., Chiappini , C., et al. 2019, , 628, A94, 10.1051/0004-6361/201935765

work page doi:10.1051/0004-6361/201935765 2019
[73]

2018, , 616, A17, 10.1051/0004-6361/201833234

Arenou , F., Luri , X., Babusiaux , C., et al. 2018, , 616, A17, 10.1051/0004-6361/201833234

work page doi:10.1051/0004-6361/201833234 2018
[74]

L., & Bailer-Jones , C

Astraatmadja , T. L., & Bailer-Jones , C. A. L. 2016 a , , 832, 137, 10.3847/0004-637X/832/2/137

work page doi:10.3847/0004-637x/832/2/137 2016
[75]

Estimating distances from parallaxes. III. Distances of two million stars in the Gaia DR1 catalogue

Astraatmadja , T. L., & Bailer-Jones , C. A. L. 2016 b , , 833, 119. 1609.07369

work page internal anchor Pith review Pith/arXiv arXiv 2016
[76]

Bailer-Jones , C. A. L. 2015, , 127, 994, 10.1086/683116

work page doi:10.1086/683116 2015
[77]

Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Mantelet , G., & Andrae , R. 2018, , 156, 58, 10.3847/1538-3881/aacb21

work page doi:10.3847/1538-3881/aacb21 2018
[78]

L., Rix , H.-W., et al

Bovy , J., Nidever , D. L., Rix , H.-W., et al. 2014, , 790, 127, 10.1088/0004-637X/790/2/127

work page doi:10.1088/0004-637x/790/2/127 2014
[79]

A., & Veljanoski , J

Breddels , M. A., & Veljanoski , J. 2018, , 618, A13, 10.1051/0004-6361/201732493

work page doi:10.1051/0004-6361/201732493 2018
[80]

2018, , 618, A93, 10.1051/0004-6361/201833476

Cantat-Gaudin , T., Jordi , C., Vallenari , A., et al. 2018, , 618, A93, 10.1051/0004-6361/201833476

work page doi:10.1051/0004-6361/201833476 2018
[81]

2020, A&A, 10.1051/0004-6361/202039834

Fabricius , C., Luri , X., Arenou , F., et al. 2020, A&A, 10.1051/0004-6361/202039834

work page doi:10.1051/0004-6361/202039834 2020
[82]

and Lang, Dustin and Goodman, Jonathan , title =

Foreman-Mackey , D., Hogg , D. W., Lang , D., & Goodman , J. 2013, , 125, 306, 10.1086/670067

work page doi:10.1086/670067 2013
[83]

2016 a , , 595, A1, 10.1051/0004-6361/201629272

Gaia Collaboration . 2016 a , , 595, A1, 10.1051/0004-6361/201629272

work page doi:10.1051/0004-6361/201629272 2016
[84]

2016 b , , 595, A2, 10.1051/0004-6361/201629512

---. 2016 b , , 595, A2, 10.1051/0004-6361/201629512

work page doi:10.1051/0004-6361/201629512 2016
[85]

2018, , 616, A1, 10.1051/0004-6361/201833051

---. 2018, , 616, A1, 10.1051/0004-6361/201833051

work page internal anchor Pith review doi:10.1051/0004-6361/201833051 2018
[86]

2020 a , arXiv:2012.01533

---. 2020 a , arXiv:2012.01533. 2012.01533

work page arXiv 2020
[87]

2020 b , arXiv:2012.02061

---. 2020 b , arXiv:2012.02061. 2012.02061

work page arXiv 2020
[88]

M., Hivon , E., Banday , A

G \'o rski , K. M., Hivon , E., Banday , A. J., et al. 2005, , 622, 759, 10.1086/427976

work page internal anchor Pith review doi:10.1086/427976 2005
[89]

J., Davies , G

Hall , O. J., Davies , G. R., Elsworth , Y. P., et al. 2019, , 486, 3569, 10.1093/mnras/stz1092

work page doi:10.1093/mnras/stz1092 2019
[90]

A., & Hartigan, P

Hartigan, J. A., & Hartigan, P. M. 1985, Ann. Statist., 13, 70, 10.1214/aos/1176346577

work page doi:10.1214/aos/1176346577 1985
[91]

Hunter, J. D. 2007, Computing In Science & Engineering, 9, 90

work page 2007
[92]

W., & Bovy , J

Leung , H. W., & Bovy , J. 2019, , 489, 2079, 10.1093/mnras/stz2245

work page doi:10.1093/mnras/stz2245 2019
[93]

2020 a , arXiv:2012.01742

Lindegren , L., et al. 2020 a , arXiv:2012.01742. 2012.01742

work page arXiv 2020
[94]

A., Hern\'andez , J., et al

Lindegren , L., Klioner , S. A., Hern\'andez , J., et al. 2020 b , A&A, 10.1051/0004-6361/202039709

work page doi:10.1051/0004-6361/202039709 2020
[95]

Luri , X., Brown , A. G. A., Sarro , L. M., et al. 2018, , 616, A9, 10.1051/0004-6361/201832964

work page doi:10.1051/0004-6361/201832964 2018
[96]

R., Schiavon , R

Majewski , S. R., Schiavon , R. P., Frinchaboy , P. M., et al. 2017, , 154, 94, 10.3847/1538-3881/aa784d

work page doi:10.3847/1538-3881/aa784d 2017
[97]

McMillan , P. J. 2018, Research Notes of the American Astronomical Society, 2, 51, 10.3847/2515-5172/aaca93

work page doi:10.3847/2515-5172/aaca93 2018
[98]

M., Bouy , H., et al

Olivares , J., Sarro , L. M., Bouy , H., et al. 2020, arXiv e-prints, arXiv:2010.00272. 2010.00272

work page arXiv 2020
[99]

2014, , 564, A49, 10.1051/0004-6361/201323037

Palmer , M., Arenou , F., Luri , X., & Masana , E. 2014, , 564, A49, 10.1051/0004-6361/201323037

work page doi:10.1051/0004-6361/201323037 2014
[100]

Queiroz , A. B. A., Anders , F., Chiappini , C., et al. 2020, , 638, A76, 10.1051/0004-6361/201937364

work page doi:10.1051/0004-6361/201937364 2020
[101]

2020, arXiv:2012.01916

Riello , M., et al. 2020, arXiv:2012.01916. 2012.01916

work page arXiv 2020
[102]

2018, , 130, 074101, 10.1088/1538-3873/aabd70

Rybizki , J., Demleitner , M., Fouesneau , M., et al. 2018, , 130, 074101, 10.1088/1538-3873/aabd70

work page doi:10.1088/1538-3873/aabd70 2018
[103]

2018, gdr2\_completeness: GaiaDR2 data retrieval and manipulation

Rybizki , J., & Drimmel , R. 2018, gdr2\_completeness: GaiaDR2 data retrieval and manipulation . 1811.018

work page 2018
[104]

Rybizki , J., Demleitner , M., Bailer-Jones , C. A. L., et al. 2020, , 132, 074501, 10.1088/1538-3873/ab8cb0

work page doi:10.1088/1538-3873/ab8cb0 2020
[105]

L., & Das , P

Sanders , J. L., & Das , P. 2018, , 481, 4093, 10.1093/mnras/sty2490

work page doi:10.1093/mnras/sty2490 2018
[106]

2017, , 472, 3979, 10.1093/mnras/stx2189

Sch \"o nrich , R., & Aumer , M. 2017, , 472, 3979, 10.1093/mnras/stx2189

work page doi:10.1093/mnras/stx2189 2017
[107]

Taylor , M. B. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 347, Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell , M. Britton , & R. Ebert , 29

work page 2005
[108]

2019, The Journal of Open Source Software, 4, 1298, 10.21105/joss.01298

Zonca , A., Singer , L., Lenz , D., et al. 2019, The Journal of Open Source Software, 4, 1298, 10.21105/joss.01298

work page doi:10.21105/joss.01298 2019
[109]

F., Speagle , J

Zucker , C., Schlafly , E. F., Speagle , J. S., et al. 2018, , 869, 83, 10.3847/1538-4357/aae97c

work page doi:10.3847/1538-4357/aae97c 2018