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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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Cites
Equation of State Calculations by Fast Computing Machines
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“As a test, we have also used the affine invariant MCMC sampler proposed byGoodman & Weare(2010), and packaged asemcee by Foreman-Mackey et al.(2013), to explore the pdf of some of our models, and found essentially identical results.”
ResultSEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE(WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION
Komatsu, E., Smith, K. M., Dunkley, J., Bennett, C. L., Gold, B., Hinshaw, G., Jarosik, N., Larson, D., Nolta, M. R., Page, L., et al. (2011) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/192/2/18 · Cited by 8,802 · cited 1×
“The critical density is ρcrit = 3H2 8πG (6) where we takeH = 70.4 km s−1 Mpc−1 from Komatsu et al.(2011).”
BackgroundInfluentialThe Structure of Cold Dark Matter Halos
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THE SEVENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
Abazajian, K. N., Adelman-McCarthy, J. K., Agüeros, M. A., Allam, S. S., Prieto, C. A., An, D., Anderson, K. S. J., Anderson, S. F., Annis, J., Bahcall, N. A., et al. (2009) · The Astrophysical Journal Supplement Series · doi:10.1088/0067-0049/182/2/543 · Cited by 5,341 · cited 1×
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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).”
BackgroundMethodInfluential
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Dynamical Histories of the Crater II and Hercules Dwarf Galaxies
Fu, S. W., Simon, J. D., & Jara, A. G. A. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab3658 · Cited by 45
Stellar 3D kinematics in the Draco dwarf spheroidal galaxy
Massari, D., Helmi, A., Mucciarelli, A., Sales, L. V., Spina, L., & Tolstoy, E. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935613 · Cited by 55
“6 kpc (McMillan 2017), for which x sub = 0 .”
BackgroundChemical and Kinematic Properties of the Galactic Disk from the LAMOST and Gaia Sample Stars
Yan, Y.-P., Du, C., Liu, S., Li, H., Shi, J., Chen, Y., Ma, J., & Wu, Z. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab287d · Cited by 49
The highest-speed local dark matter particles come from the Large Magellanic Cloud
Besla, G., Peter, A. H. G., & Garavito-Camargo, N. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/11/013 · Cited by 45
“scale lengths, mass) are listed in G19 (their table 1) and are chosen such that the disk kinematics roughly reproduce the observed rotation curve of the MW, which peaks at a value of V ∼ 240 km/s [78, 79].”
BackgroundSiegel, D. M., Agarwal, A., Barnes, J., Metzger, B. D., Renzo, M., & Villar, V. A. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac8d04 · Cited by 44
Arentsen, A., Monari, G., Queiroz, A. B. A., Starkenburg, E., Martin, N. F., Chiappini, C., Aguado, D. S., Belokurov, V. A., Carlberg, R. G., Monty, S., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1049 · Cited by 52
Simulating the Fermi Bubbles as Forward Shocks Driven by AGN Jets
Zhang, R., & Guo, F. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8bd0 · Cited by 47
Kinematics and dynamics of Gaia red clump stars
Salomon, J.-B., Bienaymé, O., Reylé, C., Robin, A. C., & Famaey, B. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038535 · Cited by 43
“…of Cepheids, that of McGaugh (2018), 233.3 ± 1.4 km s−1 based on a new analysis of the gas rotation and the determination of the distance to the Galactic centre (Gravity Collaboration et al. 2018) or the analysis of Kawata et al. (2019), 236± 3 km s−1, and McMillan (2017), 232.8 ± 3.0 km s−1.”
MethodInfluentialThe Global Stability of M33 in MOND
Banik, I., Thies, I., Famaey, B., Candlish, G., Kroupa, P., & Ibata, R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abc623 · Cited by 43
“In addition, it would also be important to consider the Milky Way, which in a MOND context must have previously interacted with M31 (Zhao et al. 2013).”
BackgroundInfluentialDynamically Tagged Groups of Very Metal-poor Halo Stars from the HK and Hamburg/ESO Surveys
Limberg, G., Rossi, S., Beers, T. C., Perottoni, H. D., Pérez-Villegas, Á., Santucci, R. M., Abuchaim, Y., Placco, V. M., Lee, Y. S., Christlieb, N., et al. (2021) · DSpace@MIT (Massachusetts Institute of Technology) · Cited by 44
Marasco, A., Fraternali, F., Lehner, N., & Howk, J. C. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1172 · Cited by 44
Streams on FIRE: Populations of Detectable Stellar Streams in the Milky Way and FIRE
Shipp, N., Panithanpaisal, N., Necib, L., Sanderson, R. E., Erkal, D., Li, T. S., Santistevan, I. B., Wetzel, A. R., Cullinane, L. R., Ji, A. P., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acc582 · Cited by 58
Testing kinematic distances under a realistic Galactic potential
Hunter, G. H., Sormani, M. C., Beckmann, J. P., Vasiliev, E., Glover, S. C. O., Klessen, R. S., Soler, J. D., Brucy, N., Girichidis, P., Göller, J., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450000 · Cited by 52
Deep Subaru Hyper Suprime-Cam Observations of Milky Way Satellites Columba I and Triangulum II*
Carlin, J. L., Sand, D. J., Muñoz, R. R., Spekkens, K., Willman, B., Crnojević, D., Forbes, D. A., Hargis, J. R., Kirby, E. N., Peter, A. H. G., et al. (2017) · The Astronomical Journal · doi:10.3847/1538-3881/aa94d0 · Cited by 43
“Had we instead used the NFW halo potential of Bovy (2015) or McMillan (2017), our results would be qualitatively similar, given that the difference between accelerations in the NFW and logarithmic halos is small in the outer regions of the Milky Way.”
MethodBird, S., Xue, X.-X., Liu, C., Flynn, C., Shen, J., Wang, J., Yang, C., Zhai, M., Ling, Z., Zhao, G., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac2036 · Cited by 49
Search for Axionic Dark Matter Using the Magnetar PSR J1745-2900
Darling, J. (2020) · Physical Review Letters · doi:10.1103/physrevlett.125.121103 · Cited by 42
Hattori, K., Valluri, M., & Vasiliev, E. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2898 · Cited by 50
Dynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds
Hatchfield, H. P., Sormani, M. C., Treß, R. G., Battersby, C., Smith, R. J., Glover, S. C. O., & Klessen, R. S. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac1e89 · Cited by 48
Milky Way total mass derived by rotation curve and globular cluster kinematics from Gaia EDR3
Wang, J., Hammer, F., & Yang, Y. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3258 · Cited by 52
High-precision chemical abundances of Galactic building blocks
Matsuno, T., Koppelman, H. H., Helmi, A., Aoki, W., Ishigaki, M. N., Suda, T., Yuan, Z., & Hattori, K. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142752 · Cited by 42
Fernandes, L., Mason, A. C., Horta, D., Schiavon, R. P., Hayes, C. R., Hasselquist, S., Feuillet, D. K., Beaton, R. L., Jönsson, H., Kisku, S. S., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3543 · Cited by 41
Exploring dark matter spike distribution around the Galactic centre with stellar orbits
Shen, Z.-Q., Yuan, G.-W., Jiang, C., Tsai, Y.-L. S., Yuan, Q., & Fan, Y.-Z. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3282 · Cited by 65
Robust cosmic-ray constraints on p -wave annihilating MeV dark matter
Boudaud, M., Lacroix, T., Stref, M., & Lavalle, J. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.99.061302 · Cited by 41
The velocity anisotropy of the Milky Way satellite system
Riley, A. H., Fattahi, A., Pace, A. B., Strigari, L. E., Frenk, C. S., Gómez, F. A., Grand, R. J. J., Marinacci, F., Navarro, J. F., Pakmor, R., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz973 · Cited by 43
“Orbit reconstruction is more challenging since the outcome is sensitive to the total and radial distribution of mass in the Milky Way, which are uncertain (Bovy 2015;McMillan 2017; see Figure 7 of Callingham et al. 2018 for a comparison of recent measurements of the total mass).”
BackgroundPfeffer, J., Trujillo-Gomez, S., Kruijssen, J. M. D., Crain, R. A., Hughes, M. E., Reina-Campos, M., & Bastian, N. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3109 · Cited by 41
“The angular momentum was calculated using the velocities and distances from Baumgardt et al. (2019), and the energies were obtained assuming the McMillan (2017) potential model of the Milky Way4.”
MethodResultGalactic potential constraints from clustering in action space of combined stellar stream data
Reino, S., Rossi, E. M., Sanderson, R. E., Sellentin, E., Helmi, A., Koppelman, H. H., & Sharma, S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab304 · Cited by 41
“…calculate the resulting rotation curves for our two-component potentials (shaded areas in Figure 12) and benchmark them against the rotation curves of galpy’s MWPotential2014 (Bovy 2015) (black dashed line) and McMillan (2017) (cyan dashed line) and the data from Eilers et al. (2019) (grey points).”
MethodCarrillo, A., Deason, A. J., Fattahi, A., Callingham, T. M., & Grand, R. J. J. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3274 · Cited by 40
The volumetric star formation law in the Milky Way
Bacchini, C., Fraternali, F., Pezzulli, G., Marasco, A., Iorio, G., & Nipoti, C. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201936559 · Cited by 20
“3.1 rather than those in McMillan (2017) model.”
BackgroundMethodInfluentialSoler, J. D., Beuther, H., Syed, J., Wang, Y., Anderson, L. D., Glover, S. C. O., Hennebelle, P., Heyer, M., Henning, T. K., Izquierdo, A. F., et al. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038882 · Cited by 40
“These simulations, run using the AREPO code, consist of a gas disk inspired by the Milky Way gas disk model of McMillan (2017) and focus on the region between 4 and 12 kpc in galactocentric radius.”
MethodA revisit of PSR J1909−3744 with 15-yr high-precision timing
Liu, K., Guillemot, L., Istrate, A., Shao, L., Tauris, T. M., Wex, N., Antoniadis, J., Chalumeau, A., Cognard, I., Desvignes, G., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2993 · Cited by 43
“Using our timing results and the model provided in McMillan (2017), we have7 Ṗ Galb = 0.0265(6) × 10−13.”
BackgroundMethodInfluentialDynamically Tagged Groups of Metal-poor Stars from the Best and Brightest Survey
Shank, D., Beers, T. C., Placco, V. M., Limberg, G., Jaques, E., Yuan, Z., Schlaufman, K. C., Casey, A. R., Huang, Y., Lee, Y. S., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac409a · Cited by 39
The Complexity of the Cetus Stream Unveiled from the Fusion of STREAMFINDER and StarGO
Yuan, Z., Malhan, K., Sestito, F., Ibata, R., Martin, N. F., Chang, J., Li, T. S., Caffau, E., Bonifacio, P., Bellazzini, M., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac616f · Cited by 43
Orbital Evidences for Dark-matter-free Milky Way Dwarf Spheroidal Galaxies
Hammer, F., Yang, Y., Arenou, F., Wang, J., Li, H., Bonifacio, P., & Babusiaux, C. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab77be · Cited by 38
Testing modified-gravity theories via wide binaries and GAIA
Pittordis, C., & Sutherland, W. J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1578 · Cited by 38
The aftermath of the Great Collision between our Galaxy and the Large Magellanic Cloud
Cautun, M., Deason, A. J., Frenk, C. S., & McAlpine, S. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3084 · Cited by 39
“…of the three galaxies are listed in Table 1 and correspond to: MW, LMC, and Andromeda halo masses from Peñarrubia et al. (2016); MW bulge and disc masses from McMillan (2017); Andromeda bulge and disc masses from Savorgnan et al. (2016); and LMC stellar mass from van der Marel et al. (2002).”
BackgroundMardini, M. K., Placco, V. M., Taani, A. A., Li, H., & Zhao, G. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab3047 · Cited by 38
The S2 Stream: the shreds of a primitive dwarf galaxy.*
Aguado, D. S., Myeong, G., Belokurov, V. A., Evans, N. W., Koposov, S. E., Prieto, C. A., Lanfranchi, G. A., Matteucci, F., Shetrone, M. D., Sbordone, L., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3250 · Cited by 38
3D hydrodynamic simulations for the formation of the Local Group satellite planes
Banik, I., Thies, I., Truelove, R., Candlish, G., Famaey, B., Pawlowski, M. S., Ibata, R., & Kroupa, P. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac722 · Cited by 38
On the Stability of Tidal Streams in Action Space
Arora, A., Sanderson, R. E., Panithanpaisal, N., Cunningham, E. C., Wetzel, A. R., & Garavito-Camargo, N. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac93fb · Cited by 44
Placco, V. M., Almeida-Fernandes, F., Holmbeck, E. M., Roederer, I. U., Mardini, M. K., Hayes, C. R., Venn, K. A., Chiboucas, K., Deibert, E., Gamen, R., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ad077e · Cited by 37
Shiva and Shakti: Presumed Proto-Galactic Fragments in the Inner Milky Way
Malhan, K., & Rix, H. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad1885 · Cited by 44
Monty, S., Belokurov, V. A., Sanders, J. L., Hansen, T. T., Sakari, C. M., McKenzie, M., Myeong, G., Davies, E. Y., Arentsen, A., & Massari, D. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1895 · Cited by 37
Lithium and beryllium in the Gaia-Enceladus galaxy
Molaro, P. P., Cescutti, G., & Fu, X. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1653 · Cited by 37
“For this calculation we use the public licensed code GALPOT following the method described in McMillan (2017), and assume a Galactic potential which includes thin and thick stellar disks, bulge, halo, and a gas disk.”
MethodThe R-process Alliance: The Peculiar Chemical Abundance Pattern of RAVE J183013.5−455510*
Placco, V. M., Santucci, R. M., Yuan, Z., Mardini, M. K., Holmbeck, E. M., Wang, X., Surman, R., Hansen, T. T., Roederer, I. U., Beers, T. C., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab99c6 · Cited by 39
Vertical motion in the Galactic disc: unwinding the snail
Frankel, N., Bovy, J., Tremaine, S. D., & Hogg, D. W. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad908 · Cited by 36
The Radcliffe Wave is oscillating
Konietzka, R., Goodman, A. A., Zucker, C., Burkert, A. M., Alves, J., Foley, M. M., Swiggum, C., Koller, M., & Miret-Roig, N. (2024) · Nature · doi:10.1038/s41586-024-07127-3 · Cited by 36
“We tested two alternative models for the Galactic potential 12,13 , finding no effect on our results.”
Nepal, S., Chiappini, C., Queiroz, A. B. A., Guiglion, G., Montalbán, J., Steinmetz, M., Miglio, A., & Khalatyan, A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449445 · Cited by 36
Galactic bar resonances inferred from kinematically hot stars in Gaia EDR3
Kawata, D., Baba, J., Hunt, J. D., Schönrich, R. A., Ciucă, I., Friske, J. K. S., Seabroke, G. M., & Cropper, M. S. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2582 · Cited by 36
“To this end, we compute the actions of our sampled stars using MCMILLAN17 (McMillan 2017) and IRRGANG13III (Model III of Irrgang et al. 2013) Galactic potentials in GALPY.”
BackgroundMethodInfluentialMass Models of the Milky Way and Estimation of Its Mass from the Gaia DR3 Data Set
Labini, F. S., Chrobáková, Ž., Capuzzo‐Dolcetta, R., & López-Corredoira, M. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acb92c · Cited by 45
Insights from super-metal-rich stars: Is the Milky Way bar young?
Nepal, S., Chiappini, C., Guiglion, G., Steinmetz, M., Pérez-Villegas, Á., Queiroz, A. B. A., Miglio, A., Dohme, P., & Khalatyan, A. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348365 · Cited by 35
A plane of high-velocity galaxies across the Local Group
Banik, I., & Zhao, H. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2596 · Cited by 57
“The flatline level of the MW rotation curve is no longer assumed equal to its amplitude vc, at the position of the Sun.8 We let the former vary with a prior of 205 ± 10 km s−1 (McGaugh 2016a), while vc, is fixed at 232.8 km s−1 (McMillan 2017).”
BackgroundInfluentialNew Nearby Hypervelocity Stars and Their Spatial Distribution from Gaia DR2
Du, C., Li, H., Yan, Y.-P., Newberg, H. J., Shi, J., Ma, J., Chen, Y., & Wu, Z. (2019) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ab328c · Cited by 37
Tracing Hercules in Galactic azimuth with Gaia DR2
Monari, G., Famaey, B., Siebert, A., Bienaymé, O., Ibata, R., Wegg, C., & Gerhard, O. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936455 · Cited by 35
“…from the Galactic centre R0 = 8.2 kpc, very close to the value of GRAVITY Collaboration (2019), Sun’s peculiar velocity w.r.t. the Local Standard of Rest (U ,V ,W ) = (11.1, 12.24, 7.25) km s−1, and Galaxy’s circular velocity at the Sun vc = 233.1 km s−1 (Schönrich et al. 2010; McMillan 2017).”
BackgroundInfluentialStellar 3D kinematics in the Draco dwarf spheroidal galaxy
Massari, D., Helmi, A., Mucciarelli, A., Sales, L. V., Spina, L., & Tolstoy, E. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935613/pdf · Cited by 38
Mardini, M. K., Placco, V. M., Meiron, Y., Ishchenko, M., Avramov, B., Mazzarini, M., Berczik, P., Sedda, M. A., Beers, T. C., Frebel, A., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abbc13 · Cited by 41
The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way
Sarkar, K. C. (2024) · The Astronomy and Astrophysics Review · doi:10.1007/s00159-024-00152-1 · Cited by 34
Tidally induced spiral arm wraps encoded in phase space
Antoja, T., Ramos, P., López-Guitart, F., Anders, F., Bernet, M., & Laporte, C. F. P. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244064 · Cited by 34
A self-consistent dynamical model of the Milky Way disc adjusted toGaiadata
Robin, A. C., Bienaymé, O., Salomon, J.-B., Reylé, C., Lagarde, N., Figueras, F., Mor, R., Fernández-Trincado, J. G., & Montillaud, J. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243686 · Cited by 34
Kinematic structures of the solar neighbourhood revealed byGaiaDR1/TGAS and RAVE
Kushniruk, I., Schirmer, T., & Bensby, T. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731147 · Cited by 34
“McMillan (2017) used a simple dynamical modelling of the Milky Way to study the origin of the Hyades stream and to check whether it could originate from a Lindblad resonance.”
MethodRotating Halo Traced by the K-giant Stars from LAMOST and Gaia
Tian, H., Liu, C., Xu, Y., & Xue, X.-X. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf6e8 · Cited by 34
Precise mass measurements for the double neutron star system J1829+2456
Haniewicz, H. T., Ferdman, R. D., Freire, P. C. C., Champion, D. J., Bunting, K., Lorimer, D. R., & McLaughlin, M. A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3466 · Cited by 34
Did Sgr cause the vertical waves in the solar neighbourhood?
Bennett, M., & Bovy, J. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab524 · Cited by 34
“However, the McMillan17 potential which has the highest frequency of all considered potentials, also has an asymmetry period roughly equivalent to that of MWP14-2 and Irrgang13I.”
BackgroundResultInfluentialSoler, J. D., Beuther, H., Syed, J., Wang, Y., Anderson, L. D., Glover, S. C. O., Hennebelle, P., Heyer, M. H., Henning, T. K., Izquierdo, A. F., et al. (2020) · Kölner Universitäts PublikationsServer (Universität zu Köln) · Cited by 34
Icarus: A Flat and Fast Prograde Stellar Stream in the Milky Way Disk
Fiorentin, P. R., Spagna, A., Lattanzi, M. G., & Cignoni, M. (2021) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/abd53d · Cited by 34
Koppelman, H. H., & Helmi, A. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202038777 · Cited by 34
“We use this value for the distance to the Galactic centre because it is consistent with the McMillan (2017) potential that we will employ later, and the same is true for the LSR velocity.”
BackgroundMethodResultInfluentialDynamical Model of the Milky Way Using APOGEE and Gaia Data
Nitschai, M. S., Eilers, A., Neumayer, N., Cappellari, M., & Rix, H. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac04b5 · Cited by 36
“In addition, we combined that with an axisymmetric bulge (McMillan 2017; Bissantz & Gerhard 2002).”
BackgroundMethodInfluentialEvidence for sub-Chandrasekhar Type Ia supernovae from the last major merger
Sanders, J. L., Belokurov, V. A., & Man, K. T. F. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1951 · Cited by 34
“This catalogue assumes the MWPOTENTIAL2014 from Bovy (2015) whilst for the other data sets we have assumed the McMillan (2017) potential.”
BackgroundMethodInfluentialZhao, J., Shao, L., Cao, Z., & Ma, B.-Q. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.100.064034 · Cited by 39
Radial halo substructure in harmony with the Galactic bar
Dillamore, A. M., Belokurov, V. A., & Evans, N. W. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1789 · Cited by 37
Constraining the mass of the Local Group
Carlesi, E., Hoffman, Y., Sorce, J. G., & Gottlöber, S. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw3073 · Cited by 31
The time evolution of the Milky Way’s oxygen abundance gradient
Mollá, M., Díaz, Á. I., Cavichia, O., Gibson, B. K., Maciel, W. J., Costa, R. D. D., Ascasíbar, Y., & Few, C. G. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2877 · Cited by 33
Finding the Remnants of the Milky Way's Last Neutron Star Mergers
Wu, M.-R., Banerjee, P., Metzger, B. D., Martínez-Pinedo, G., Aramaki, T., Burns, E., Hailey, C. J., Barnes, J., & Karagiorgi, G. S. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab2593 · Cited by 33
The Gaia–ESO Survey: Carbon Abundance in the Galactic Thin and Thick Disks *
Franchini, M., Morossi, C., Marcantonio, P. D., Chávez, M., Adibekyan, V., Bayo, A., Bensby, T., Bragaglia, A., Calura, F., Duffau, S., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab5dc4 · Cited by 33
Probing the Milky Way’s Dark Matter Halo for the 3.5 keV Line
Sicilian, D., Cappelluti, N., Bülbül, E., Civano, F., Moscetti, M., & Reynolds, C. S. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abbee9 · Cited by 42
“Furthermore, the systematic uncertainty introduced by the choice of model parameters prevents us from excluding correspondence to all NFW profiles, such as the McMillan (2017) profile shown in Figure 11.”
BackgroundMethodInfluentialZhao, G., & Chen, Y. (2021) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-020-1645-5 · Cited by 33
DESI Early Data Release Milky Way Survey value-added catalogue
Koposov, S. E., Prieto, C. A., Cooper, A. P., Li, T. S., Silva, L. J. B. E., Kim, B., Carrillo, A., Dey, A., Manser, C. J., Nikakhtar, F., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1842 · Cited by 33
The Formation and Evolution of Galactic Disks with APOGEE and the Gaia Survey
Li, C., Zhao, G., Zhai, M., & Jia, Y. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac50f · Cited by 32
“This wedge only exists under the hypothesis that the potential of the Galaxy is axisymmetric (Binney 2016; Binney & McMillan 2016).”
BackgroundThe Imprint of Spiral Arms on the Galactic Rotation Curve
McGaugh, S. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab479b · Cited by 34
Gravitational deflection of massive particles in Schwarzschild-de Sitter spacetime
He, G., Zhou, X., Feng, Z.-W., Mu, X., Wang, H., Li, W., Pan, C., & Lin, W. (2020) · The European Physical Journal C · doi:10.1140/epjc/s10052-020-8382-z · Cited by 33
The volumetric star formation law in the Milky Way
Bacchini, C., Fraternali, F., Pezzulli, G., Marasco, A., Iorio, G., & Nipoti, C. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201936559/pdf · Cited by 32
High-precision chemical abundances of Galactic building blocks
Matsuno, T., Dodd, E., Koppelman, H. H., Helmi, A., Ishigaki, M. N., Aoki, W., Zhao, J., Yuan, Z., & Hattori, K. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243609 · Cited by 32
Probing the Galactic halo with RR Lyrae stars – II. The substructures of the Milky Way
Wang, F., Zhang, H.-W., Xue, X.-X., Huang, Y., Liu, G.-C., Zhang, L., & Yang, C.-Q. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac874 · Cited by 32
The warm-hot circumgalactic medium of the Milky Way as seen by eROSITA
Locatelli, N. T., Ponti, G., Zheng, X., Merloni, A., Becker, W., Comparat, J., Dennerl, K., Freyberg, M. J., Sasaki, M., & Yeung, M. C. H. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347061 · Cited by 31
Mapping the anisotropic Galactic stellar halo with blue horizontal branch stars
Amarante, J. A. S., Koposov, S. E., & Laporte, C. F. P. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450351 · Cited by 35
On the existence of a very metal-poor disc in the Milky Way
Zhang, H., Arentsen, A., & Belokurov, V. A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1887 · Cited by 35
Neutrino clustering in the Milky Way and beyond
Mertsch, P., Parimbelli, G., de Salas, P. F., Gariazzo, S., Lesgourgues, J., & Sergio Pastor, B. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/01/015 · Cited by 42
Neutrino clustering in the Milky Way and beyond
Mertsch, P., Parimbelli, G., de Salas, P. F., Gariazzo, S., Julien Lesgourgues, A., & Sergio Pastor, B. (2020) · RWTH Publications (RWTH Aachen) · Cited by 31
Zepeda, J., Beers, T. C., Placco, V. M., Shank, D., Gudin, D., Hirai, Y., Mardini, M. K., Pifer, C., Catapano, T., & Calagna, S. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acbbcc · Cited by 34
A Walk on the Retrograde Side (WRS) project
Ceccarelli, E., Massari, D., Mucciarelli, A., Bellazzini, M., Nunnari, A., Cusano, F., Lardo, C., Romano, D., Ilyin, I. V., & Stokholm, A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348332 · Cited by 32
The escape velocity curve of the Milky Way in modified Newtonian dynamics
Banik, I., & Zhao, H. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2350 · Cited by 33
“…escape velocity curves that arises because both are determined by the same potential Φ. ∂ ( 1 2 vesc 2 ) ∂r = −∂Φ ∂r (20) = − vc 2 r (21) α ≡ − ∂Ln vesc ∂Ln r = ( vc vesc )2 (22) If we assume that vc, = 232.8 km/s (McMillan 2017), then we expect α = 0.200 for a local escape velocity of 521 km/s.”
BackgroundMethodInfluentialOrbital evidences for dark-matter-free Milky Way dwarf spheroidal galaxiesPreprint
Hammer, F., Yang, Y., Arenou, F., Wang, J., Li, H., Bonifacio, P., & Babusiaux, C. (2020) · HAL · Cited by 31
Clues to the origin of Fermi bubbles from O viii/O vii line ratio
Sarkar, K. C., Nath, B. B., & Sharma, P. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx314 · Cited by 30
Geometry-driven and dark-matter-sustained Milky Way rotation curves with Gaia DR3
Beordo, W., Crosta, M., Lattanzi, M. G., Re Fiorentin, P., & Spagna, A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae855 · Cited by 30
Abe, H., Abe, S., Acciari, V. A., Aniello, T., Ansoldi, S., Antonelli, L. A., Engels, A. A., Arcaro, C., Artero, M., Asano, K., et al. (2023) · Physical Review Letters · doi:10.1103/physrevlett.130.061002 · Cited by 52
An artificial neural network to discover hypervelocity stars: candidates in Gaia DR1/TGAS
Marchetti, T., Rossi, E. M., Kordopatis, G., Brown, A. G. A., Rimoldi, A., Starkenburg, E., Youakim, K., & Ashley, R. P. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1304 · Cited by 30
“Our choice for the mass of the bulge is significantly higher compared to the latest observational constraints (Bland-Hawthorn & Gerhard 2016; McMillan 2017), therefore we integrate each candidate assuming a bulge mass equal to half the previous adopted value: Mb = 1.7 × 1010 M , keeping fixed all…”
InfluentialThe Flattening Metallicity Gradient in the Milky Way’s Thin Disk
Vickers, J. J., Shen, J., & Li, Z. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac27a9 · Cited by 30
Ishikawa, H. T., Aoki, W., Hirano, T., Kotani, T., Kuzuhara, M., Omiya, M., Hori, Y., Kokubo, E., Kudo, T., Kurokawa, T., et al. (2022) · The Astronomical Journal · doi:10.3847/1538-3881/ac3ee0 · Cited by 30
Why do black holes trace bulges (& central surface densities), instead of galaxies as a whole?
Hopkins, P. F., Wellons, S., Anglés‐Alcázar, D., Faucher‐Giguère, C., & Grudić, M. Y. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3458 · Cited by 30
A transiting brown dwarf in a 2 hour orbit
El-Badry, K., Burdge, K. B., van Roestel, J., & Rodriguez, A. C. (2023) · The Open Journal of Astrophysics · doi:10.21105/astro.2307.15729 · Cited by 29
Kinematics and dynamics of the Galactic bar revealed by Gaia long-period variables
Zhang, H., Belokurov, V. A., Evans, N. W., Kane, S. G., & Sanders, J. L. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2023 · Cited by 36
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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