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Cited by 14Stellar, planetary, and galactic studiesGalaxies: Formation, Evolution, PhenomenaAstrophysical Phenomena and Observations

Assessing the robustness of the Galactic rotation curve inferred from the Jeans equations using Gaia DR3 and cosmological simulations

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Koop, Orlin, Antoja, Teresa, Helmi, Amina, Callingham, Thomas M., Laporte, Chervin F. P.·2024·Astronomy & Astrophysics
DOI 10.1051/0004-6361/202450911
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Abstract

Context. Several authors have recently applied Jeans modelling to Gaia-based datasets to infer the circular velocity curve for the Milky Way. These works have consistently found evidence for a continuous decline in the rotation curve beyond ~15 kpc, which may indicate the existence of a light dark matter (DM) halo. Aims. Using a large sample of Gaia DR3 data, we aim to derive the rotation curve of the Milky Way using the Jeans equations, and to quantify the role of systematic effects, both in the data and those inherent to the Jeans methodology under the assumptions of axisym-metry and time independence. Methods. We used data from the Gaia DR3 radial velocity spectrometer sample, supplemented with distances inferred through Bayesian frameworks, to determine the radial variation of the second moments of the velocity distribution for stars close to the Galactic plane. We used these profiles to determine the rotation curve using the Jeans equations under the assumption of axisym-metry and explored how they vary with azimuth and position above and below the plane of the Galactic disc. We applied the same methodology to an N-body simulation of a Milky Way-like galaxy impacted by a satellite akin the Sagittarius dwarf, and to the Auriga suite of cosmological simulations. Results. The circular velocity curve we infer for the Milky Way is consistent with previous findings out to ~15 kpc, where our statistics are robust. Due to the larger number of stars in our sample, we are able to reveal evidence of disequilibrium and deviations from axisymmetry closer in. For example, we find that the second moment of VR flattens out at R ≳ 12.5 kpc, and that the second moment of Vϕ is different above and below the plane for R ≳ 11 kpc. Our exploration of the simulations indicates that these features are typical of galaxies that have been perturbed by external satellites. From the simulations, we also estimate that the difference between the true circular velocity curve and that inferred from Jeans equations can be as high as 15%, but that it is likely of the order of 10% for the Milky Way. This is higher than the systematic uncertainties associated with the observations or those linked to most modelling assumptions when using the Jeans equations. However, if the density of the tracer population were truncated at large radii instead of being exponential as often assumed, this could lead to the erroneous conclusion of a steeply declining rotation curve. Conclusions. We find that steady-state axisymmetric Jeans modelling becomes less robust at large radii, indicating that particular caution must be exercised when interpreting the rotation curve inferred in those regions. A more careful and sophisticated approach may be necessary for precision measurements of the DM content of our Galaxy.

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  • Koop et al. (2024) find that the difference between the true circular-speed curve and the Jeans-inferred one can reach about 10-15% in Milky Way-like systems, and caution that a radially truncated tracer density can produce a spuriously steep apparent decline at large R even when the underlying rotation curve is essentially flat.

    “A complementary Gaia DR3 Jeans-equation reanalysis by Koop et al. (2024), using both observational data and N -body simulations including a Sagittarius-like perturber, finds that the difference between the true circular-speed curve and the Jeans-inferred one can reach ∼ 10-15% in MW-like systems, and cautions specifically that a radially truncated tracer density can produce a spuriously steep”

    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 Koop et al. (2024)

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Authors
Koop, O., Antoja, T., Helmi, A., Callingham, T. M., & Laporte, C. F. P.
Affiliations
  • University of Groningen (NL)
  • Institut de Ciències del Cosmos (ES)
ORCID
Venue
Astronomy & Astrophysics
Publisher
EDP Sciences
Published
2024-12
Volume
692
Pages
A50
ISSN
  • 0004-6361 (ISSN-L)
  • 1432-0746
DOI
10.1051/0004-6361/202450911
OpenAlex
W4403632602
Cited by
14
References
88
Citations by year
2026: 5 · 2025: 7 · 2024: 2
FWCI
2.64
Type
journal article
Language
en
Open access
Licence
Locations
  • Astronomy and Astrophysics (publishedVersion, cc-by)
  • DIGITAL.CSIC (Spanish National Research Council (CSIC)) (acceptedVersion, other-oa)
  • arXiv (Cornell University) (submittedVersion, cc-by)
  • University of Groningen research database (University of Groningen / Centre for Information Technology) (submittedVersion, cc-by)
  • arXiv (Cornell University) (cc-by)
Funders
  • European Space Agency
  • European Commission (CNS2022-135232, 13039/501100011033, 501100011033, PID2021-125451NA-I00)
  • Universitat de Barcelona (CEX2019-000918-M)
  • European Regional Development Fund (MCIN/AEI/10, 13039/501100011033, RYC2018-025968-I, CEX2019-000918-M, 501100011033, MICIU/AEI/10)
  • Agencia Estatal de Investigación (501100011033, RYC2018-025968-I, 13039, CEX2019-000918-M, .13039/501100011033, PID2021-125451NA-I00, AEI/10, CNS2022-135232)
  • Institut de Ciències del Cosmos (CEX2019–000918–M)
  • European Social Fund (501100011033)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Keywords
Milky Way rotation curve, Jeans equation, dark matter halos, axial symmetry, velocity dispersion anisotropy, Sagittarius dwarf galaxy, satellite orbit perturbations, Auriga simulations, Gaia DR3, systematic uncertainties, stellar kinematics, Galactic disc

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