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The mass distribution and gravitational potential of the Milky Way
Open accessAbstract
We present mass models of the Milky Way created to fit observational constraints and to be consistent with expectations from theoretical modelling. The method used to create these models is that demonstrated in our previous study, and we improve on those models by adding gas discs to the potential, considering the effects of allowing the inner slope of the halo density profile to vary, and including new observations of maser sources in the Milky Way amongst the new constraints. We provide a best-fitting model, as well as estimates of the properties of the Milky Way. Under the assumptions in our main model, we find that the Sun is R0 = 8.20 ± 0.09 kpc from the Galactic Centre, with the circular speed at the Sun being v0 = 232.8 ± 3.0 km s−1; and that the Galaxy has a total stellar mass of (54.3 ± 5.7) × 109 M⊙, a total virial mass of (1.30 ± 0.30) × 1012 M⊙ and a local dark-matter density of 0.40 ± 0.04 GeV cm−3, where the quoted uncertainties are statistical. These values are sensitive to our choice of priors and constraints. We investigate systematic uncertainties, which in some cases may be larger. For example, if we weaken our prior on R0, we find it to be 7.97 ± 0.15 kpc and that v0 = 226.8 ± 4.2 km s−1. We find that most of these properties, including the local dark-matter density, are remarkably insensitive to the assumed power-law density slope at the centre of the dark-matter halo. We find that it is unlikely that the local standard of rest differs significantly from that found under assumptions of axisymmetry. We have made code to compute the force from our potential, and to integrate orbits within it, publicly available.
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“Such studies argue that the Galactic halo has a very high concentration, typically ∼ 14 or higher”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as McMillan 2017
Experimental — accuracy not yet measuredThe source backs part of the claim, not all of it — or backs it for a different population, condition or comparison.
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“This stellar mass is in good agreement with estimates for the MW (e.g. Bovy & Rix 2013; McMillan 2017, and Section 5)”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as McMillan 2017
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“and even more flexible formulae, such as the generalised NFW profile (gNFW, which has been used to model the MW halo - McMillan 2017; Karukes et al. 2019b), struggle to describe the radial profile of the contracted halo.”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as McMillan 2017
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“They correspond to an HI mass of 1 . 1 × 10 10 M ⊙ and a molecular gas mass of 10 percent of the HI mass.”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as McMillan 2017
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Citations
Cites
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ResultSEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
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MethodSimulations of the formation, evolution and clustering of galaxies and quasars
Springel, V., White, S. D. M., Jenkins, A. R., Frenk, C. S., Yoshida, N., Gao, L., Navarro, J. F., Thacker, R. J., Croton, D., Helly, J. C., et al. (2005) · Nature · doi:10.1038/nature03597 · Cited by 5,060 · cited 1×
“The relationship betweenM∗ and Mv was determined by ‘abundance matching’ of the galaxy stellar masses found byLi & White (2009) with the halo virial masses found in the Millennium simulations (Springel et al. 2005; Boylan-Kolchin et al. 2009).”
MethodEnsemble samplers with affine invariance
Goodman, J. B., & Weare, J. (2010) · Communications in Applied Mathematics and Computational Science · doi:10.2140/camcos.2010.5.65 · Cited by 3,075
corner.py: Scatterplot matrices in Python
Foreman-Mackey, D. T. (2016) · The Journal of Open Source Software · doi:10.21105/joss.00024 · Cited by 2,183 · cited 1×
“The corner plots were created with thecorner.py package (Foreman-Mackey 2016).”
MethodLocal kinematics and the local standard of rest
Schönrich, R. A., Binney, J. J., & Dehnen, W. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16253.x · Cited by 1,934 · cited 5×
“…a R0 in an axisymmetric approximation of the true potential (i.e. what we find in this study), and the velocity of a closed orbit,and therefore a theoretical 0 km s−1 dispersion population, in the Solar neighbourhood (which is what is found by local measurementslike that of Schönrich et al. 2010).”
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“On the other hand, simulations suggest that thick disks could be produced through secular radial migration of stars induced by spiral arms (Roskar et al. 2008; Schoenrich & Binney 2009; Curir et al. 2012) and flaring combined with inside-out disk formation (Minchev et al. 2017).”
BackgroundMethodInfluentialAcceleration relations in the Milky Way as differentiators of modified gravity theories
Islam, T., & Dutta, K. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.101.084015 · Cited by 10
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Beane, A., Sanderson, R. E., Ness, M., Johnston, K., Grion Filho, D., Mac Low, M., Anglés-Alcázar, D., Hogg, D., & Laporte, C. F. P. (2019) · MPG.PuRe (Max Planck Society) · Cited by 10
Koppelman, H. H., Hagen, J. H. J., & Helmi, A. (2021) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/202039390/pdf · Cited by 10
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“We use the model provided in McMillan (2016) to compute stellar mass density along a line of sight.”
MethodWeakly supervised anomaly detection in the Milky Way
Pettee, M. N., Thanvantri, S., Nachman, B. P., Shih, D., Buckley, M. R., & Collins, J. H. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3663 · Cited by 10
Sattler, N., Pinna, F., Neumayer, N., Falcón‐Barroso, J., Martig, M., Gadotti, D. A., van de Ven, G., & Minchev, I. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad275 · Cited by 9
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de Isídio, N., Menéndez‐Delmestre, K., Gonçalves, T. S., Grossi, M., Rodrigues, D. C., Garavito-Camargo, N., Araujo-Carvalho, A. E., Beaklini, P. P. B., Cavalcante-Coelho, Y., Cortesi, A., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad53c8 · Cited by 9
emPDF : inferring the Milky Way mass with data-driven distribution function in phase space
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The Hubble Missing Globular Cluster Survey
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Abac, A., Abouelfettouh, I., Acernese, F., Ackley, K., Adamcewicz, C., Adhicary, S., Adhikari, D., Adhikari, N., Adhikari, R. X., Adkins, V. K., et al. (2025) · Physical review. D/Physical review. D. · doi:10.1103/wjdz-jdby · Cited by 9
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Parthasarathy, M., Matsuno, T., & Aoki, W. (2020) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psaa097 · Cited by 9
“We adopt 8.2 kpc as the distance between the Sun and the Galactic center (McMillan 2017), 0.025 kpc as the vertical offset of the Sun (Jurić et al. 2008).”
MethodInfluentialGaia Early Data Release 3. Acceleration of the solar system from Gaia astrometry
Bertone, S., & Mignard, F. (2020) · UCL Discovery (University College London) · doi:10.13016/m2pt0u-lozb · Cited by 9
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The Galactic Bulge Exploration. III. Calcium Triplet Metallicities for RR Lyrae Stars
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The distance to the Galactic centre: globular clusters and SEKBO RR Lyrae survey stars
Griv, E., Gedalin, M., & Jiang, I. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz006 · Cited by 9
Griv, E., Gedalin, M., Pietrukowicz, P., Majaess, D., & Jiang, I. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2845 · Cited by 9
Monty, S., Yong, D., Massari, D., McKenzie, M., Myeong, G., Buder, S., Karakas, A. I., Freeman, K. C., Marino, A. F., Belokurov, V. A., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1154 · Cited by 9
Cosmic ray antihelium from a strongly coupled dark sector
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The dynamics of Galactic centre pulsars: constraining pulsar distances and intrinsic spin-down
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“This software was based on Dehnen & Binney (1998) and the details of the computation are given in McMillan (2017).”
BackgroundMethodResultInfluentialMeasuring the local dark matter density in the laboratory
Kavanagh, B. J., Emken, T., & Catena, R. (2021) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.104.083023 · Cited by 8
Petač, M. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.102.123028 · Cited by 11
The formation history of the Milky Way disc with high-resolution cosmological simulations
Giammaria, M., Spagna, A., Lattanzi, M. G., Murante, G., Fiorentin, P. R., & Valentini, M. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab136 · Cited by 9
“…baryonic mass distribution (considering test particles that would move in an axisymmetric gravitational potentialΦ according to Newtonian theory) represents one of the main line of evidence of the presence of dark matter (DM) in haloes (e.g. Iocco et al. 2015; McMillan 2017; de Salas et al. 2019).”
BackgroundCharacterization of high-velocity stars in the S-PLUS internal fourth data release
Quispe-Huaynasi, F., Roig, F., Placco, V. M., Silva, L. J. B. E., Daflon, S., Pereira, C. B., Kanaan, A., de Oliveira, C. M., Ribeiro, T., & Schoenell, W. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3610 · Cited by 8
Bernet, M., Ramos, P., Antoja, T., Monari, G., & Famaey, B. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348410 · Cited by 8
Brown, S. T., Fattahi, A., McCarthy, I. G., Font, A. S., Oman, K. A., & Riley, A. H. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1378 · Cited by 8
Mapping the Milky Way with LAMOST – IV. The large Galactic disc extending to 35 kpc
Tian, H., Liu, C., Li, J., & Zhang, B. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1247 · Cited by 8
Discovery of an Extremely r-process-enhanced Thin-disk Star with [Eu/H] = +0.78
Xie, X., Shi, J., Yan, H.-L., Chen, T.-Y., Prieto, C. A., Beers, T. C., Liu, S., Li, C., Ding, M.-Y., Tang, Y.-J., et al. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad5ffd · Cited by 9
Placco, V. M., Gupta, A. F., Almeida-Fernandes, F., Logsdon, S. E., Rajagopal, J., Holmbeck, E. M., Roederer, I. U., Costa, J. D., Fernandez, P., Golub, E., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8646 · Cited by 8
Chemical Abundance Gradients in Open Clusters from the Gaia/LAMOST Sample
Yang, G., Zhao, J., Yang, Y., Liu, N., Luo, Y., & Zhao, G. (2025) · The Astronomical Journal · doi:10.3847/1538-3881/adba45 · Cited by 8
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“The gravitational potential of the MW includes contributions from six components (McMillan 2016): a DM halo, a bulge, two stellar discs, and two gas discs, while the potential of the LMC is modeled as that corresponding to a Hernquist density profile (Erkal & Belokurov 2020).”
The messy merger of a large satellite and a Milky Way-like galaxy
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“When deriving velocity, we adopt vLSR = 232.8 km s−1 (McMillan 2017).”
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Almeida-Fernandes, F., Placco, V. M., Rocha–Pinto, H. J., Fernandes, M. B., Limberg, G., Silva, L. J. B. E., Amarante, J. A. S., Perottoni, H. D., Overzier, R., Schoenell, W., et al. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1561 · Cited by 10
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Self-citationLehmann, C., Feltzing, S., Feuillet, D. K., & Kordopatis, G. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1736 · Cited by 8
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“For instance, axisymmetric models developed by Piffl et al. (2014); McMillan (2017); Binney & Wong (2017) use HIand CO velocities, maser data, Sgr A* proper motions, the globular cluster system, the velocity distribution in the SN, SDSS star counts in different colours, RAVE data, detailed MW…”
MethodLacroix, T., Facchinetti, G., Pérez-Romero, J., Stref, M., Lavalle, J., Maurin, D. A., & Sánchez-Conde, M. Á. (2022) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2022/10/021 · Cited by 8
Binary Clusters: Theory and Observations
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The Influence of the Galactic Bar on the Dynamics of Globular Clusters
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“[26], first we modelled the Milky Way using the axisymmetric potential described by McMillan [45](McMillan17).”
BackgroundMethodInfluentialChen, I., Kongsore, M., & Tilburg, K. V. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/07/037 · Cited by 8
“) We assume that the DM distribution in the MW follows a NavarroFrenk-White (NFW) profile [89] with a fiducial scale radius Rs = 18 kpc and a local DM density ρ = 10−2M /pc3 [84]”
MethodImpact of an Active Sgr A* on the Synthesis of Water and Organic Molecules throughout the Milky Way
Liu, C., Chen, X., & Du, F. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/aba758 · Cited by 9
Existence of the Metal-rich Stellar Halo and High-velocity Thick Disk in the Galaxy
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The reduced proper motion selected halo: Methods and description of the catalogue
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The likelihood of undiscovered globular clusters in the outskirts of the Milky Way
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“Note that clusters AM 4 and Laevens 3 are not bound to MWPotential2014 and AM 4 is not bound to the McMillan (2017) model, given the most recent estimates of their proper motions.”
BackgroundMethodInfluentialDestruction of Galaxies as a Cause of the Appearance of Stellar Streams
Tutukov, A. V., Vereshchagin, S. V., & Сизова, М. Д. (2021) · Astronomy Reports · doi:10.1134/s106377292111007x · Cited by 8
New constraints on decaying dark matter from INTEGRAL/SPI
Fischer, S. M., Malyshev, D., Ducci, L., & Santangelo, A. E. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad304 · Cited by 7
The oldest stars with low neutron-capture element abundances and origins in ancient dwarf galaxies
Andales, H. D., Figueiredo, A. S., Fienberg, C. G., Mardini, M. K., & Frebel, A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae670 · Cited by 7
The chemical evolution of the Milky Way thin disk using solar twins
Plotnikova, A., Spina, L., Ratcliffe, B., Casali, G., & B, G. C. A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451167 · Cited by 7
Stellar Streams Reveal the Mass Loss of Globular Clusters
Chen, Y., Li, H., & Gnedin, O. Y. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/adaf93 · Cited by 7
Larsen, J. R., Mosumgaard, J. R., Aguirre, V. S., Lundkvist, M. S., Christensen-Dalsgaard, J., Winther, M. L., Stokholm, A., Li, Y., Slumstrup, D., Kjeldsen, H., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453554 · Cited by 7
NGC 1851A: Revealing an ongoing three-body encounter in a dense globular cluster
Dutta, A., Freire, P. C. C., Gautam, T., Wex, N., Ridolfi, A., Champion, D. J., Krishnan, V. V., Chen, C. ‐. R., Cadelano, M., Kramer, M., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452433 · Cited by 7
Thomsen, J. S., Miglio, A., Brogaard, K., Montalbán, J., Tailo, M., van Rossem, W. E., Casali, G., Jones, D., Arentoft, T., Casagrande, L., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453347 · Cited by 7
A simulation-based inference approach to the dynamics of the MW–LMC system - validation
Brooks, R. A. N., Sanders, J. L., Dillamore, A. M., Garavito-Camargo, N., & Price-Whelan, A. M. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf2111 · Cited by 7
A Walk on the Retrograde Side (WRS) project
Ceccarelli, E., Massari, D., Palla, M., Mucciarelli, A., Bellazzini, M., & Helmi, A. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202556685 · Cited by 7
Leo, M. D., Massari, D., Bellazzini, M., Mucciarelli, A., Acosta-Tripailao, B., & Nipoti, C. (2026) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202556723 · Cited by 7
Can planet 9 be an axion star?
Di, H., & Shi, H. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.108.103038 · Cited by 7
“38GeV / cm 3 [54].”
Exploring theex-situcomponents withinGaiaDR3
Li, Z., Zhao, G., Zhang, R., Xue, X.-X., Chen, Y., & Amarante, J. A. S. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3817 · Cited by 7
On the Galactic radio signal from stimulated decay of axion dark matter
Dev, P. S. B., Ferrer, F., & Okawa, T. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/04/045 · Cited by 7
“…[140] where subscripts denote either stars (s) or axion stars (AS), ⟨ v 2s ⟩ and ⟨ v 2AS ⟩ are the corresponding mean-squared velocities, and ρ s = ρ b + ρ d , thin + ρ d , thick is the density of ordinary stars which receives contributions from the bulge and from the thin and thick discs [63,64].”
Compositions of the Hercules–Aquila Cloud and Virgo Overdensity
Ye, D., Du, C., Deng, M., Liao, J., Huang, Y., Shi, J., & Ma, J. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1655 · Cited by 7
Exploration of Halo Substructures in Integrals-of-motion Space with Gaia Data Release 3
Liu, H., Du, C., Ye, D., Zhang, J., & Deng, M. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8352 · Cited by 7
A particle's perspective on screening mechanisms
Muñoz, S. S. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/12/052 · Cited by 12
“For a realistic illustration of this scenario, we would also have to consider other galaxy components, such as dark matter 6 and the bulge [77], but we will neglect them in this illustration for simplicity.”
The Solar System’s passage through the Radcliffe wave during the middle Miocene
Maconi, E., Alves, J., Swiggum, C., Ratzenböck, S., Großschedl, J. E., Köhler, P., Miret-Roig, N., Meingast, S., Konietzka, R., Zucker, C., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452061 · Cited by 10
Identifying Galactic Substructures in 5D Space Using All-sky RR Lyrae Stars in Gaia DR3
Sun, S. S., Wang, F., Zhang, H., Xue, X.-X., Huang, Y., Zhang, R., Rix, H., Li, X., Liu, G., Zhang, L., et al. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/ad9de0 · Cited by 7
Bayer, M., Starkenburg, E., Thomas, G. F., Martin, N. F., Helmi, A., Byström, A., de Boer, T. J. L., Fernández-Alvar, E., Gwyn, S., Ibata, R., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202554131 · Cited by 7
Two Substructures in the nearby Stellar Halo Found in Gaia and RAVE
Li, H., Du, C., Yang, Y., Newberg, H. J., Ma, J., Shi, J., & Yun-song Piao, A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8733 · Cited by 7
“Here we adopt recent VLSR = 232.8 km s−1(McMillan 2017), V = 11 km s−1(Bland-Hawthorn & Gerhard 2016).”
BackgroundMethodInfluentialRevisit NGC 5466 tidal stream withGaia, SDSS/SEGUE, and LAMOST
Yang, Y., Zhao, J., Ishigaki, M. N., Zhou, J., Yang, C., Xue, X.-X., Ye, X., & Zhao, G. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac860 · Cited by 7
Existence of tidal tails for the globular cluster NGC 5824
Yang, Y., Zhao, J., Ishigaki, M. N., Chiba, M., Yang, C., Xue, X.-X., Ye, X., & Zhao, G. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243976 · Cited by 7
The Tully–Fisher relation and the Bosma effect
Labini, F. S., Marzo, G. D., Straccamore, M., & Comerón, S. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3278 · Cited by 7
Bandyopadhyay, A., Beers, T. C., Ezzeddine, R., Sivarani, T., Nayak, P. K., Pandey, J. C., Saraf, P., & Susmitha, A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae613 · Cited by 7
An overlooked source of uncertainty in the mass of the Milky Way
Oman, K. A., & Riley, A. H. (2024) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slae042 · Cited by 7
Stellar streams in chameleon gravity
Naik, A. P., Evans, N. W., Puchwein, E., Zhao, H., & Davis, A.-C. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.102.084066 · Cited by 7
“[41], which is designed to fit a number of recent kinematic constraints on the Milky Way matter distribution.”
BackgroundProbing the Halo Gas Distribution in the Inner Galaxy with Fermi Bubble Observations
Zhang, R.-Y., & Guo, F.-L. (2021) · Astrophysical Journal · doi:10.3847/1538-4357/abfdb1 · Cited by 5
“The hot gas is assumed to be in hydrostatic equilibrium with temperature T= 2.32× 106 K (0.2 keV) in the galactic potential, which is determined by an updated MW mass model proposed in (McMillan 2017, see Z20 for details).”
MethodInfluentialRevisiting pulsar velocities using Gaia Data Release 2
Yang, M., Dai, S., Li, D., Tsai, C.-W., Zhu, W.-W., & Zhang, J. (2021) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/21/6/141 · Cited by 7
“Previously, Tauris et al. (2017) used the Galactic model of McMillan (2017) and Monte Carlo simulations to estimate the velocity of DNS LSR and its dispersion.”
MethodFacchinetti, G., Lavalle, J., & Stref, M. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.106.083023 · Cited by 9
Young stars raining through the galactic halo: the nature and orbit of price-whelan 1
Bellazzini, M., Ibata, R., Martin, N. F., Malhan, K., Marasco, A., & Famaey, B. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2788 · Cited by 7
“This corresponds to 〈VLSR〉 = 272 ± 10 km/s in the Local Standard of Rest, and VGSR = 84 ± 10 km/s in the Galactic standard of rest, adopting the solar motion by Schönrich, Binney & Dehnen (2010) and the circular speed of the Sun from McMillan (2017).”
BackgroundFirst measurement of the triaxiality of the inner dark matter halo of the Milky Way
Woudenberg, H. C., & Helmi, A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451743 · Cited by 13
Discovery of a pair of very metal-poor stars enriched in neutron-capture elements
da Silva, A. R., & Smiljanić, R. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202453295 · Cited by 9
An Actinide-boost Star Discovered in the Gaia-Sausage-Enceladus
Lin, Y., Li, H., Jiang, R., Aoki, W., Honda, S., He, Z., Zhang, R., Li, Z., & Zhao, G. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/adc8a3 · Cited by 8
Gaps in stellar streams as a result of globular cluster flybys
Ferrone, S. M., Montuori, M., Matteo, P. D., Mastrobuono-Battisti, A., Ibata, R., Bianchini, P., Александрович, Х. С., Leclerc, N., Hottier, C., Stein, E., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202553923 · Cited by 6
Dynamical streams in the local stellar halo
Dillamore, A. M., Sanders, J. L., Belokurov, V. A., & Zhang, H. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf965 · Cited by 11
The double neutron star PSR J1946+2052
Meng, L., Freire, P. C. C., Stovall, K., Wex, N., Miao, X., Zhu, W., Krämer, M., Cordes, J. M., Hu, H., Jiang, J., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202555689 · Cited by 6
Racca, M., Hansen, T. T., Roederer, I. U., Placco, V. M., Frebel, A., Beers, T. C., Ezzeddine, R., Holmbeck, E. M., Sakari, C. M., Monty, S., et al. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202556947 · Cited by 8
The dark side of early galaxies: geko uncovers dark-matter fractions at z ∼ 4 − 6
Danhaive, A. L., Tacchella, S., Bunker, A. J., Curtis-Lake, E., de Graaff, A., D’Eugenio, F., Duan, Q., Egami, E., Eisenstein, D. J., Johnson, B. D., et al. (2026) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stag119 · Cited by 12
Metadata
- Authors
- McMillan, P. J.
- Affiliations
- Lund University (SE)
- Corresponding author
- McMillan, Paul J.
- ORCID
- McMillan, Paul J.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2016-10-26
- Volume
- 465
- Issue
- 1
- Pages
- 76-94
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2485876312
- Cited by
- 1,099
- References
- 128
- Citations by year
- 2026: 104 · 2025: 165 · 2024: 154 · 2023: 126 · 2022: 120 · 2021: 121 · 2020: 118 · 2019: 88 · 2018: 64 · 2017: 36 · 2016: 3
- FWCI
- 30.41
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Lund University Publications (Lund University) (submittedVersion)
- HighWire Press Open Archive (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- Milky Way mass distribution, gravitational potential, dark matter halos, stellar mass, virial mass, local dark matter density, local standard of rest, halo density profiles, gas discs, orbit integration, axial symmetry
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