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Gaia Data Release 3: Properties and validation of the radial velocities

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Katz, D., Sartoretti, P., Guerrier, A., Panuzzo, P., Seabroke, G. M., Thévenin, F., Cropper, M., Benson, K. +42 more·2023·Astronomy & Astrophysics
DOI 10.1051/0004-6361/202244220
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Abstract

Context. Gaia Data Release 3 ( Gaia DR3) contains the second release of the combined radial velocities. It is based on the spectra collected during the first 34 months of the nominal mission. The longer time baseline and the improvements of the pipeline made it possible to push the processing limit from G RVS = 12 in Gaia DR2 to G RVS = 14 mag. Aims. We describe the new functionalities implemented for Gaia DR3, the quality filters applied during processing and post-processing, and the properties and performance of the published velocities. Methods. For Gaia DR3, several functionalities were upgraded or added to the spectroscopic pipeline. The calibrations were improved in order to better model the temporal evolution of the straylight and of the instrumental point spread function (PSF). The overlapped spectra, which were mostly discarded in Gaia DR2, are now handled by a dedicated module. The hot star template mismatch, which prevented publication of hot stars in Gaia DR2, is largely mitigated now, down to G RVS = 12 mag. The combined radial velocity of stars brighter than or equal to G RVS = 12 mag is calculated in the same way as in Gaia DR2, that is, as the median of the epoch radial velocity time series. The combined radial velocity of the fainter stars is measured from the average of the cross-correlation functions. Results. Gaia DR3 contains the combined radial velocities of 33 812 183 stars. With respect to Gaia DR2, the temperature interval has been expanded from T eff ∈ [3600, 6750] K to T eff ∈ [3100, 14 500] K for the bright stars ( G RVS ≤ 12 mag) and [3100, 6750] K for the fainter stars. The radial velocities sample a significant part of the Milky Way: they reach a few kiloparsecs beyond the Galactic centre in the disc and up to about 10−15 kpc vertically into the inner halo. The median formal precision of the velocities is 1.3 km s −1 at G RVS = 12 and 6.4 km s −1 at G RVS = 14 mag. The velocity zeropoint exhibits a small systematic trend with magnitude that starts around G RVS = 11 mag and reaches about 400 m s −1 at G RVS = 14 mag. A correction formula is provided that can be applied to the published data. The Gaia DR3 velocity scale agrees satisfactorily with APOGEE, GALAH, GES, and RAVE; the systematic differences mostly remain below a few hundred m s −1 . The properties of the radial velocities are also illustrated with specific objects: open clusters, globular clusters, and the Large Magellanic Cloud. For example, the precision of the data allows mapping the line-of-sight rotational velocities of the globular cluster 47 Tuc and of the Large Magellanic Cloud.

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  • The Gaia mission measures parallaxes and proper motions for ∼1.5 billion stars, with parallax precision σπ ≈ 0.01-0.1 mas, and radial velocities for ∼33 million objects in DR3.

    “The Gaia mission (Gaia Collaboration et al., 2016), launched in December 2013, measures parallaxes and proper motions for ∼ 1 . 5 billion stars, with parallax precision σϖ ≈ 0 . 01-0 . 1 mas, and radial velocities for ∼ 33 million objects in DR3 (Katz et al., 2023).”

    From The rotation curve of the Milky Way: State of the art, the Keplerian decline debate, and implications for dark matter (2026) · cites this paper as Katz et al., 2023

    The Introduction describes about 1.5 billion Gaia targets, and the Conclusions report radial velocities for 33,812,183 stars in DR3 (p. 23). The cited paper does not establish that parallaxes and proper motions are measured for approximately 1.5 billion stars or give the claimed parallax-precision range; its precision figures concern radial velocities. (LLM, conf=0.86)

    Experimental — accuracy not yet measured

  • Gaia DR3 parallax precision depends on magnitude, colour, position, scanning law, and source quality; a single polynomial in G does not describe the catalogue.

    “Gaia DR3 parallax precision depends on magnitude, colour, position, scanning law, and source quality; a single polynomial in G does not describe the catalogue.”

    From The rotation curve of the Milky Way: State of the art, the Keplerian decline debate, and implications for dark matter (2026) · cites this paper as Katz et al., 2023

    Section 8 (A5, pp. 16–17) discusses the precision of Gaia DR3 radial velocities, including variation with magnitude, stellar properties, sky position, and the scanning law—not parallax precision. Searches for parallax precision and a polynomial in G found no passage addressing the claim about the parallax catalogue. (LLM, conf=0.77)

    Experimental — accuracy not yet measured

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Authors
Katz, D., Sartoretti, P., Guerrier, A., Panuzzo, P., Seabroke, G. M., Thévenin, F., Cropper, M., Benson, K., Blomme, R., Haigron, R., Marchal, O., Smith, M., Baker, S., Chemin, L., Damerdji, Y., David, M., Dolding, C., Frémat, Y., Gosset, E., Janßen, K., Jasniewicz, G., Lobel, A., Plum, G., Samaras, N., Snaith, O., Soubiran, C., Vanel, O., Zwitter, T., Antoja, T., Arenou, F., Babusiaux, C., Brouillet, N., Caffau, E., Di Matteo, P., Fabre, C., Fabricius, C., Fragkoudi, F., Haywood, M., Huckle, H. E., Hottier, C., Lasne, Y., Leclerc, N., Mastrobuono-Battisti, A., Royer, F., Teyssier, D., Zorec, J., Crifo, F., Jean-Antoine Piccolo, A., Turon, C., & Viala, Y.
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2023-06
Volume
674
Pages
A5
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/202244220
OpenAlex
W3098034015
Cited by
351
References
114
Citations by year
2026: 52 · 2025: 78 · 2024: 84 · 2023: 52 · 2022: 13 · 2021: 29 · 2020: 26 · 2019: 16 · 2018: 1
FWCI
22.51
Type
journal article
Language
en
Open access
Licence
Locations
  • Astronomy and Astrophysics (publishedVersion, cc-by)
  • DIGITAL.CSIC (Spanish National Research Council (CSIC)) (acceptedVersion)
  • HAL (submittedVersion, cc-by)
  • ORBi (University of Liège) (submittedVersion, other-oa)
  • Lund University Publications (Lund University) (submittedVersion)
Funders
  • National Science Foundation (299543, CEX2019-000918-M)
  • National Aeronautics and Space Administration (UIDB/04434/2020, UIDP/04434/2020, LP2014-17, 299543)
  • UK Space Agency (ST/N000641/1, ST/N001117/1, ST/K000756/1)
  • European Space Agency (65316, 4000115263/15/NL/IB)
  • University of Cambridge
  • University of Leicester
  • University College London
  • European Commission (FP7-SPACE-2013-1, 895174, 320360, 2014‐2020, 10.13039/501100011033, TIN2015-65316-P, MICIN/AEI/10.13039/501100011033, 13039/501100011033, 255267, 501100011033, HORIZON2020, 745617, 647208, 682115, 606740, 264895, /AEI/10.13039/501100011033, 695099, 101004214, 951549, 716155, 687378, 834148, RTI2018-095076-B-C21)
  • European Science Foundation
  • University of Edinburgh
  • University of Bristol
  • European Cooperation in Science and Technology (CA18104)
  • Science Foundation Ireland
  • Agence Nationale de la Recherche (ANR-15-CE31-0007, 2017-, ANR-19-CE31-0017, ANR-10-IDEX-0001, ANR‐19, ANR-10-IDEX0001-02., ANR-15-CE31-0012, ANR18, ANR-10-IDEX, ANR-14-CE33-0014, 0014-01, ANR-10, IDEX-0001-02, 834148, ANR-18-CE31-0006, ANR-14-CE33)
  • Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung (137523, 65316, ANR-10-IDEX-0001-02, 121059, 194638)
  • Swedish National Space Agency
  • Academy of Finland (325805, 328654, #307157, #299543, 336546, 345115, 128840)
  • Belgian Federal Science Policy Office
  • Generalitat de Catalunya (10.13039/501100011033, 2014-SGR-1051, 501100011033, MICIN/AEI/10.13039/501100011033, CEX2019-000918-M, TIN2015-65316)
  • Centre National d’Etudes Spatiales (682115, IN2P3)
  • Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO-M-614.061.414)
  • Magyar Tudományos Akadémia (DL 57/2016, LP2014-17, LP2018-7, KKP-137523)
  • Agenzia Spaziale Italiana (I/037/08/0, 2013/030/I.0, 2014-025-R.1.2015, 025-R.1.2015, I/008/10/0, 2018-24-HH.0, 2014-025-R.0, 2019-3, 2014-049-R.0, I/058/10/0)
  • Liverpool John Moores University
  • Magnus Ehrnroothin Säätiö (2014-025-R.0)
  • Javna Agencija za Raziskovalno Dejavnost RS (P1-0188)
  • Tel Aviv University
  • Ministerstwo Edukacji i Nauki (DIR/WK/2018/12, 2014-2020, 2016-17, DL 57/2016)
  • Centre National de la Recherche Scientifique
  • Ministerio de Ciencia e Innovación (IJC2019-04862-I, MICIN AEI/10.13039/501100011033/, .13039/501100011033, 10.13039, IJC2019-04862-, 2016-17, / AEI/10, TIN2015-65316P, TIN2015-65316, 10.13039/501100011033/, CEX2019-000918- M, 501100011033, CEX2019, RYC2018-025968-I, /AEI/10.13039/ 501100011033)
  • Istituto Nazionale di Astrofisica (I/008/10/0, 2016-17-I.0, 2014-025-R.1.2015, KKP-137523, 2014-049-R.0/1/2, 2014-025-R.0, 2013/030/I.0)
  • Universitat de Barcelona (CEX2019-000918-M)
  • Université de Bordeaux (ANR-10-IDEX)
  • Barcelona Supercomputing Center
  • Xunta de Galicia (ED481A, ED431G, ED431B)
  • Nemzeti Kutatási Fejlesztési és Innovációs Hivatal (KKP137523)
  • Université de Franche-Comté
  • Instituto de Astrofísica de Canarias
  • Observatoire de Paris, Université de Recherche Paris Sciences et Lettres
  • Science and Technology Facilities Council (UIDB/04434/2020, ST/L006561/1, ST/S001980/1, UIDP/04434/2020, /10.13039/501100011033, IN2P3, ST/S000984/1, DIR/WK/2018/12, ST/S001948/1, ST/T00147X/1, ST/X005933/1, ST/S002103/1)
  • Fundação para a Ciência e a Tecnologia (DL-57/2016, 01-0145, UIDB/04434/2020 and UIDP/04434/2020, POCI-01-0145-FEDER-030389, 57/2016, POCI-01-0145, PTDC/FIS-AST/30389/2017, 2019-3, UIDP/04434/2020, UIDB/04434/2020, POCI-01-0145-FEDER-, COMPETE_2020, POCI-01-, 10.13039/501100011033, /2017, DL 57/2016/CP1364/CT0006, MICIN/AEI/10.13039/501100011033)
  • European Regional Development Fund (2014-2020’, POCI-01-0145-FEDER- 030389, POCI-01, 10.13039/501100011033, UIDP/04434/2020, 13039/501100011033, COMPETE2020, MICIN/AEI/10.13039/501100011033, UIDB/04434/2020, AEI/10.13039/501100011033, RYC2018-025968-I, CEX2019-000918-M, 501100011033, DL 57/2016, RTI2018, 57/ 2016, PTDC/FIS-AST/30389/2017, RTI2018-095076-B-C21, POCI-01-0145- FEDER, AyA2017-84089)
  • Agencia Estatal de Investigación (AEI//10.13039/501100011033/, 501100011033, RYC2018-025968-I, 10.13039/501100011033, 13039, CEX2019-000918-M, RTI2018-095076-B-C22, .13039/501100011033, IJC2019-04862-I, 10.13039, AEI/10, MICIN/AEI/10.13039/501100011033)
  • Institut National de Physique Nucléaire et de Physique des Particules
  • Institut de Ciències del Cosmos (CEX2019–000918–M)
  • Zentrum für Informationsdienste und Hochleistungsrechnen, Technische Universität Dresden
  • HORIZON EUROPE Excellent Science
  • European Social Fund (MICIN/AEI/10.13039/501100011033, 20142020, DL 57/2016, ED431G-2019/01, ED481A-2019/155, 501100011033, AEI/10.13039/501100011033)
  • FP7 Space
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Instrumentation › Astronomy and Astrophysical Research
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
Gaia DR3, radial velocity, Gaia RVS, stellar spectroscopy, cross correlation function, hot stars, Milky Way kinematics, stellar populations, stellar effective temperature, Galactic halo, Galactic disc, stellar distances, stellar parallax

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