Mass models of the Milky Way

McMillan, Paul J.

doi:10.1111/j.1365-2966.2011.18564.x

Cited by 789Stellar, planetary, and galactic studiesGalaxies: Formation, Evolution, PhenomenaAstrophysical Phenomena and Observations

Mass models of the Milky Way

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McMillan, Paul J.·2011·Monthly Notices of the Royal Astronomical Society

DOI 10.1111/j.1365-2966.2011.18564.x

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Abstract

We present a simple method for fitting parametrized mass models of the Milky Way to observational constraints. We take a Bayesian approach which allows us to take into account input from photometric and kinematic data, and expectations from theoretical modelling. This provides us with a best-fitting model, which is a suitable starting point for dynamical modelling. We also determine a probability density function on the properties of the model, which demonstrates that the mass distribution of the Galaxy remains very uncertain. For our choices of parametrization and constraints, we find disc scalelengths of 3.00 ± 0.22 and 3.29 ± 0.56 kpc for the thin and thick discs, respectively, a solar radius of 8.29 ± 0.16 kpc and a circular speed at the Sun of 239 ± 5 km s−1, a total stellar mass of 6.43 ± 0.63 × 1010 M⊙, a virial mass of 1.26 ± 0.24 × 1012 M⊙ and a local dark matter density of 0.40 ± 0.04 GeV cm−3. We find some correlations between the best-fitting parameters of our models (for example, between the disc scalelengths and the solar radius), which we discuss. The chosen disc scaleheights are shown to have little effect on the key properties of the model.

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The exact value of the disc scale-height does not significantly affect the inferred MW mass model.
“We note that the exact value of z d does not significantly affect the inferred MW mass model - see e.g. McMillan (2011).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as McMillan 2011
Section 5.1 says changing the disc scaleheights has very little impact on the overall structure of the Galaxy models: bulge and virial masses are virtually unchanged. It also reports a significant change in how disc mass is divided between the thin and thick discs, so the unqualified claim is broader than the result. (LLM, conf=0.85)
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Binney J. J., McMillan P. J., 2011, MNRAS, preprint (arXiv:1101.0747) · arXiv
Burnett B. C. M., 2010, PhD thesis, Univ. Oxford

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“1 M ⊙ ; McMillan 2011, 2017) lies at the boundary of the above mass limit, it was uncertain whether our Galaxy contains such a CGM around it.”
Background
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Authors: McMillan, P. J.
Affiliations: University of Oxford (GB)
Corresponding author: McMillan, Paul J.
ORCID: McMillan, Paul J.
Venue: Monthly Notices of the Royal Astronomical Society
Publisher: Oxford University Press (OUP)
Published: 2011-04-15
Volume: 414
Issue: 3
Pages: 2446-2457
ISSN: 0035-8711 (ISSN-L)
DOI: 10.1111/j.1365-2966.2011.18564.x
OpenAlex: W1921289443
Cited by: 789
References: 73
Citations by year: 2026: 10 · 2025: 30 · 2024: 47 · 2023: 31 · 2022: 45 · 2021: 51 · 2020: 59 · 2019: 57 · 2018: 56 · 2017: 69 · 2016: 91 · 2015: 82 · 2014: 71 · 2013: 48 · 2012: 34
FWCI: 27.01
Type: journal article
Language: en
Open access: bronze
doi.org
Locations: Monthly Notices of the Royal Astronomical Society (publishedVersion)
arXiv (Cornell University) (submittedVersion)
Lund University Publications (Lund University) (submittedVersion)
arXiv (Cornell University)
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: Bayesian parameter estimation, solar radius, stellar mass, virial mass, dark matter density

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