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Estimating the dark matter halo mass of our Milky Way using dynamical tracers
Open accessAbstract
The mass of the dark matter halo of the Milky Way can be estimated by fitting analytical models to the phase-space distribution of dynamical tracers. We test this approach using realistic mock stellar haloes constructed from the Aquarius N-body simulations of dark matter haloes in the Λ cold dark matter cosmology. We extend the standard treatment to include a Navarro–Frenk–White potential and use a maximum likelihood method to recover the parameters describing the simulated haloes from the positions and velocities of their mock halo stars. We find that the estimate of halo mass is highly correlated with the estimate of halo concentration. The best-fitting halo masses within the virial radius, R200, are biased, ranging from a 40 per cent underestimate to a 5 per cent overestimate in the best case (when the tangential velocities of the tracers are included). There are several sources of bias. Deviations from dynamical equilibrium can potentially cause significant bias; deviations from spherical symmetry are relatively less important. Fits to stars at different galactocentric radii can give different mass estimates. By contrast, the model gives good constraints on the mass within the half-mass radius of tracers even when restricted to tracers within 60 kpc. The recovered velocity anisotropies of tracers, β, are biased systematically, but this does not affect other parameters if tangential velocity data are used as constraints.
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Cites
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Self-citationThe Structure of Cold Dark Matter Halos
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Self-citationA Universal Density Profile from Hierarchical ClusteringPreprint
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Self-citationMinuit - a system for function minimization and analysis of the parameter errors and correlations
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Self-citationThe Aquarius Project: the subhaloes of galactic haloes
Springel, V., Wang, J., Vogelsberger, M., Ludlow, A. D., Jenkins, A. R., Helmi, A., Navarro, J. F., Frenk, C. S., & White, S. D. M. (2008) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.14066.x · Cited by 1,990
Self-citationToo big to fail? The puzzling darkness of massive Milky Way subhaloes
Boylan-Kolchin, M., Bullock, J. S., & Kaplinghat, M. (2011) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1111/j.1745-3933.2011.01074.x · Cited by 1,395
Ground-based and Airborne Instrumentation for Astronomy
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Dark matter self-interactions and small scale structure
Tulin, S., & Yu, H.-B. (2018) · Physics Reports · doi:10.1016/j.physrep.2017.11.004 · Cited by 1,111
The milky way total mass profile as inferred from Gaia DR2
Cautun, M., Benítez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1017 · Cited by 332
“While there are many Galactic mass estimates (e.g. see the compilations in Wang et al. 2015; Callingham et al. 2019b), we choose the Callingham et al. result since it has several advantages compared to other studies: i) the method had been thoroughly tested with multiple hydrodynamic simulations,…”
MethodResultSelf-citationThe Milky Way total mass profile as inferred from Gaia DR2
Cautun, M., Benitez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2019) · arXiv · doi:10.48550/arxiv.1911.04557 · Cited by 335
“While there are many Galactic mass estimates (e.g. see the compilations in Wang et al. 2015; Callingham et al. 2019b), we choose the Callingham et al. result since it has several advantages compared to other studies: i) the method had been thoroughly tested with multiple hydrodynamic simulations,…”
MethodResultSelf-citationVogelsberger, M., Zavala, J., Cyr-Racine, F.-Y., Pfrommer, C., Bringmann, T., & Sigurdson, K. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1076 · Cited by 257
“1 of Wang et al. 2015).”
Lyman- α constraints on ultralight scalar dark matter: Implications for the early and late universe
Kobayashi, T., Murgia, R., Andrea De Simone, A., Iršič, V., & Viel, M. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.96.123514 · Cited by 238
The apostle project: Local Group kinematic mass constraints and simulation candidate selection
Fattahi, A., Navarro, J. F., Sawala, T., Frenk, C. S., Oman, K. A., Crain, R. A., Furlong, M., Schaller, M., Schaye, J., Theuns, T., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2970 · Cited by 214
“A review of the literature cited above shows that these methods produce a range of estimates (spanning a factor of 2–3) of the individual masses of the MW and M31 and/or the total mass of the LG (see Wang et al. 2015, for a recent compilation).”
BackgroundSelf-citationGalactic Dark Matter Halos and Globular Cluster Populations. III. Extension to Extreme Environments
Harris, W. E., Blakeslee, J. P., & Harris, G. L. H. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/836/1/67 · Cited by 178
“Finally then, Mh ' 1.1×1012M , which is well within the mix of estimates obtained from a wide variety of methods involving satellite dynamics and Local Group timing arguments (see, e.g. Wang et al. 2015; Eadie & Harris 2016, for compilations and comparisons).”
BackgroundInfluentialThe mass of the Milky Way from satellite dynamics
Callingham, T. M., Cautun, M., Deason, A. J., Frenk, C. S., Wang, W., Gómez, F. A., Grand, R. J. J., Marinacci, F., & Pakmor, R. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz365 · Cited by 166
“Although over the past decades a large amount of effort has been dedicated to inferring the Galactic halo mass, its value remains uncertain to within a factor of two, with most mass estimates ranging from 0.5 to 2.5 × 1012M (e.g. Wang et al. 2015, and our Fig.”
BackgroundResultInfluentialSelf-citationEvidence for an Intermediate-mass Milky Way from Gaia DR2 Halo Globular Cluster Motions
Watkins, L. L., van der Marel, R. P., Sohn, S. T., & Wyn Evans, N. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab089f · Cited by 189
Mapping the Stellar Halo with the H3 Spectroscopic Survey
Conroy, C., Bonaca, A., Cargile, P., Johnson, B., Caldwell, N., Naidu, R., Zaritsky, D., Fabricant, D., Moran, S., Rhee, J., et al. (2019) · Astrophysical Journal · doi:10.3847/1538-4357/ab38b8 · Cited by 99
“The total mass of the Galaxy is unknown to a factor of two (Wang et al. 2015), which is a major limiting factor when placing the Galaxy in a cosmological context.”
BackgroundThe fraction of dark matter within galaxies from the IllustrisTNG simulations
Lovell, M. R., Pillepich, A., Genel, S., Nelson, D., Springel, V., Pakmor, R., Marinacci, F., Weinberger, R., Torrey, P., Vogelsberger, M., et al. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2339 · Cited by 149
“…of the MW halo mass itself (Kahn & Woltjer 1959; Kahn & Woltjer 1959; Sales et al. 2007a,b; Li & White 2008; Busha et al. 2011; Deason et al. 2012; Wang et al. 2012;González et al. 2013; Boylan-Kolchin et al. 2013; Cautun et al. 2014; Peñarrubia et al. 2014; Piffl et al. 2014; Wang et al. 2015a).”
BackgroundMethodResultWang, W., Han, J., Cautun, M., Li, Z., & Ishigaki, M. N. (2020) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-019-1541-6 · Cited by 160
Self-citationThe total satellite population of the Milky Way
Newton, O., Cautun, M., Jenkins, A. R., Frenk, C. S., & Helly, J. C. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1085 · Cited by 133
“To investigate the sensitivity of the inferred total satellite luminosity function to the MW halo mass, we repeated our analysis for two extreme mass values, 0.5 × 1012 M and 2.0 × 1012 M , corresponding roughly to lower and upper bounds for the MW halo mass (e.g. Wang et al. 2015).”
BackgroundMethodInfluentialSelf-citationAstrophysical constraints on resonantly produced sterile neutrino dark matter
Schneider, A. (2016) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2016/04/059 · Cited by 127
THE CATERPILLAR PROJECT: A LARGE SUITE OF MILKY WAY SIZED HALOS
Griffen, B. F., Ji, A. P., Dooley, G. A., Gómez, F. A., Vogelsberger, M., O’Shea, B. W., & Frebel, A. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/818/1/10 · Cited by 120
“…following mass and isolation criteria: • Halos were selected between 0.7 × 1012 M ≤Mvir ≤ 3 × 1012 M (Smith et al. 2007, Xue et al. 2008, Tollerud et al. 2012, Boylan-Kolchin et al. 2013, Sohn et al. 2013, Piffl et al. 2014, Guo et al. 2015, Penarrubia et al. 2015, see Wang et al. 2015 for review).”
BackgroundInfluentialSystematics in virial mass estimators for pressure-supported systems
Errani, R., Peñarrubia, J., & Walker, M. G. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2505 · Cited by 114
“A different approach is discussed by Wang et al. (2015), who fit analytical distribution functions to observables extracted from stellar tracers embedded in DM haloes of the Aquarius (Springel et al. 2008) simulations.”
MethodLimits on Population III star formation with the most iron-poor stars
de Bennassuti, M., Salvadori, S., Schneider, R., Valiante, R., & Omukai, K. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2687 · Cited by 122
“…MMW = 1012 M at z = 0, which is in agreement with current measurements and uncertainties: 1.26+0.24−0.24 × 1012 M (McMillan 2011), 0.9+0.4−0.3 × 1012 M (Kafle et al. 2012), 0.80+0.31−0.16 × 1012 M (Kafle et al. 2014, see also Wang et al. 2015 for the different methods adopted to infer the DM mass).”
BackgroundInfluentialThe stellar-to-halo mass relation of GAMA galaxies from 100 deg 2 of KiDS weak lensing data
van Uitert, E., Cacciato, M., Hoekstra, H., Brouwer, M. M., Sifón, C., Viola, M. G., Baldry, I. K., Bland‐Hawthorn, J., Brough, S., Brown, M. J. I., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw747 · Cited by 107
“1 of Wang et al. 2015).”
Planes of satellite galaxies: when exceptions are the rule
Cautun, M., Bose, S., Frenk, C. S., Guo, Q., Han, J., Hellwing, W. A., Sawala, T., & Wang, W. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1557 · Cited by 104
“…consistent with the mass of the MW and M31 halo (e.g. Fardal et al. 2013; Piffl et al. 2014; Cautun et al. 2014b,a; Veljanoski et al. 2014; González, Kravtsov & Gnedin 2014, for a compilation of other measurements and discussions of systematic effects see Courteau et al. 2014; Wang et al. 2015).”
BackgroundSelf-citationThe Caterpillar Project: a large suite of Milky Way sized halos
Griffen, B. F., Ji, A. P., Dooley, G. A., Gómez, F., Vogelsberger, M., O'Shea, B., & Frebel, A. (2016) · MPG.PuRe (Max Planck Society) · Cited by 101
Gaia DR2 in 6D: searching for the fastest stars in the Galaxy
Marchetti, T., Rossi, E. M., & Brown, A. G. A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2592 · Cited by 111
Synthetic catalog of black holes in the Milky Way
Olejak, A., Belczynski, K., Bulik, T., & Sobolewska, M. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201936557 · Cited by 61
Missing dark matter in dwarf galaxies?
Oman, K. A., Navarro, J. F., Sales, L. V., Fattahi, A., Frenk, C. S., Sawala, T., Schaller, M., & White, S. D. M. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1251 · Cited by 97
“The Milky Way sits near the peak of this relation and, at feff ∼ 0.2 (for a baryonic mass of order ∼5 × 1010 and a virial mass of 1.5 × 1012 M , Rix & Bovy 2013; Wang et al. 2015), it is considered something of an outlier where galaxy formation has proceeded particularly efficiently.”
BackgroundInfluentialSelf-citationSatellite galaxies in semi-analytic models of galaxy formation with sterile neutrino dark matter
Lovell, M. R., Bose, S., Boyarsky, A. M., Cole, S., Frenk, C. S., González-Pérez, V., Kennedy, R., Oleg Ruchayskiy, C., & Smith, A. G. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1317 · Cited by 85
“…the kinematics of bright Milky Way satellites, (Sales et al. 2007a,b; Busha et al. 2011; Wang et al. 2012; Boylan-Kolchin et al. 2013; González et al. 2013; Cautun et al. 2014) and the timing argument (Kahn & Woltjer 1959; Li & White 2008); for a more comprehensive list see Wang et al. (2015).”
BackgroundMethodSelf-citationThe Circular Velocity Curve of the Milky Way from 5–25 kpc Using Luminous Red Giant Branch Stars
Zhou, Y., Li, X., Huang, Y., & Zhang, H. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acadd9 · Cited by 85
“However, due to the lack of accurate proper motions and the limited precision of distances, the constructed RC profiles have suffered both large systematic and random errors (e.g., Wang et al. 2015, 2020).”
BackgroundMethodThe mass of the Milky Way out to 100 kpc using halo stars
Deason, A. J., Erkal, D., Belokurov, V. A., Fattahi, A., Gómez, F. A., Grand, R. J. J., Pakmor, R., Xue, X.-X., Liu, C., Yang, C., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3984 · Cited by 91
A comparison of Galactic electron density models using PyGEDM
Price, D. C., Flynn, C., & Deller, A. T. (2021) · Publications of the Astronomical Society of Australia · doi:10.1017/pasa.2021.33 · Cited by 80
On the run: mapping the escape speed across the Galaxy with SDSS
Williams, A. A., Belokurov, V. A., Casey, A. R., & Evans, N. W. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx508 · Cited by 77
“If the true speeds of Triangulum II, Tucana II, Grus 1, Bootes III and Hercules are close to √ 3 v||, then they are likely to be unbound. equations, but this generally comes at the cost of large systematic uncertainties that arise from the chosen form of the model (Wang et al. 2015).”
BackgroundZavala, J., Lovell, M. R., Vogelsberger, M., & Burger, J. D. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.100.063007 · Cited by 76
The multiplicity and anisotropy of galactic satellite accretion
Shao, S., Cautun, M., Frenk, C. S., Grand, R. J. J., Gómez, F. A., Marinacci, F., & Simpson, C. M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty343 · Cited by 71
“The wide mass range is motivated by the large uncertainties in the total mass of the MW (e.g. Fardal et al. 2013; Cautun et al. 2014b; Piffl et al. 2014; Wang et al. 2015; Han et al. 2016) and the need to have a large sample of such systems.”
BackgroundSelf-citationEquilibrium models of the Milky Way mass are biased high by the LMC
Erkal, D., Belokurov, V. A., & Parkin, D. L. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2840 · Cited by 82
“We note that in this work we neglected the effect of substructure in the stellar halo which can cause mass estimates to be biased low by as much as ∼ 40% (e.g. Yencho et al. 2006; Wang et al. 2015).”
BackgroundDark matter–radiation interactions: the structure of Milky Way satellite galaxies
Schewtschenko, J. A., Baugh, C. M., Wilkinson, R., Bœhm, C., Pascoli, S., & Sawala, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1078 · Cited by 70
“The severity of the small-scale problems can be reduced if one considers the mass of the MW, which impacts the selection of MWlike haloes in the simulations but remains difficult to determine (Wang et al. 2012; Cautun et al. 2014; Piffl et al. 2014; Wang et al. 2015).”
BackgroundClosing in on resonantly produced sterile neutrino dark matter
Cherry, J. F., & Horiuchi, S. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.95.083015 · Cited by 67
The Imprint of Cosmic Reionization on the Luminosity Function of Galaxies
Bose, S., Deason, A. J., & Frenk, C. S. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacbc4 · Cited by 65
“…is defined as a halo of mass at z = 0 in the range 7× 1011 ≤M200/M ≤ 2× 1012 (e.g. Smith et al. 2007; Deason et al. 2012; Boylan-Kolchin et al. 2013, see Wang et al. 2015 for a comprehensive list of references); an LMC-mass host is defined as a halo of mass in the range 1.5 × 1011 ≤ M200/M ≤ 3.5 ×…”
BackgroundInfluentialSelf-citationConstraining the Milky Way Mass Profile with Phase-space Distribution of Satellite Galaxies
Li, Z.-Z., Qian, Y.-Z., Han, J., Li, T. S., Wang, W., & Jing, Y. P. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab84f0 · Cited by 77
“As shown by Wang et al. (2015) and Han et al. (2016a), unjustified assumptions (e.g., constant velocity anisotropy) in constructing the DF may lead to substantially biased results.”
BackgroundSelf-citationFornasa, M., Cuoco, A., Zavala, J., Gaskins, J., Sánchez-Conde, M. Á., Gómez-Vargas, G. A., Komatsu, E., Linden, T., Prada, F., Zandanel, F., et al. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.94.123005 · Cited by 60
Alignments between galaxies, satellite systems and haloes
Shao, S., Cautun, M., Frenk, C. S., Gao, L., Crain, R. A., Schaller, M., Schaye, J., & Theuns, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1247 · Cited by 61
“The wide mass range is motivated by the large uncertainties in the mass of the MW (e.g. Fardal et al. 2013; Cautun et al. 2014; Piffl et al. 2014; Wang et al. 2015; Han et al. 2016) and the need to have a large sample of such systems.”
BackgroundSelf-citationAddressing the too big to fail problem with baryon physics and sterile neutrino dark matter
Lovell, M. R., González-Pérez, V., Bose, S., Boyarsky, A. M., Cole, S., Frenk, C. S., & Oleg Ruchayskiy, C. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx621 · Cited by 58
“The adoption of the Wang et al. (2015b) correction factor improves the probability by over a factor of two as compared to the CDM-Vmax values, with the peak in the probability distribution located as high as 1.4×1012M⊙.”
BackgroundMethodInfluentialSelf-citationA fresh look into the interacting dark matter scenario
Escudero, M., Lopez-Honorez, L., Mena, O., Palomares-Ruiz, S., & Villanueva-Domingo, P. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2018/06/007 · Cited by 58
“Notice that we show the results as a function of the MW mass M200 MW, within its expected mass range [172].”
BackgroundThe mass of our Galaxy from satellite proper motions in the Gaia era
Fritz, T. K., Cintio, A. D., Battaglia, G., Brook, C. B., & Taibi, S. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1040 · Cited by 69
“We therefore compare to hydrodynamical simulations, for which we use the NIHAO and MaGICC simulations, considering only those simulated MWs within 1σ of the MW’ observed vcirc value at 19 kpc.”
BackgroundMethodInfluentialBAYESIAN MASS ESTIMATES OF THE MILKY WAY: THE DARK AND LIGHT SIDES OF PARAMETER ASSUMPTIONS
Eadie, G. M., & Harris, W. E. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/829/2/108 · Cited by 54
Dooley, G. A., Peter, A. H. G., Yang, T., Willman, B., Griffen, B. F., & Frebel, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1900 · Cited by 54
“Since no model was calibrated exclusively to the MW satellites, and there is uncertainty in the mass of the Milky Way from ≈ 0.5 − 2.5 × 1012 M (Wang et al. 2015), an exact agreement with the MW luminosity function is not expected.”
MethodInfluentialSynthetic catalog of black holes in the Milky Way
Olejak, A., Belczyński, K., Bulik, T., & Sobolewska, M. A. (2018) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201936557/pdf · Cited by 55
The stellar mass, star formation rate and dark matter halo properties of LAEs atz ∼ 2
Kusakabe, H., Shimasaku, K., Ouchi, M., Nakajima, K., Goto, R., Hashimoto, T., Konno, A., Harikane, Y., Silverman, J. D., & Capak, P. L. (2017) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/psx148 · Cited by 50
“…(LMC: Mh ∼ 0.2– 3× 1011 M⊙; van der Marel & Kallivayalil 2014; Peñarrubia et al. 2016, and references therein), not in MW-like halos (Mh ∼ 8× 10 11–2× 1012 M⊙; e.g., Wilkinson & Evans 1999; Kafle et al. 2014; Eadie et al. 2015, summarized in figure 1 in Wang et al. 2015), as shown in figure 12.”
BackgroundInfluentialKoch, A., Grebel, E. K., & Martell, S. L. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834825 · Cited by 52
“…hand, many studies have attempted weighing the entire halo (i.e., dark plus stellar) from a variety of tracers (e.g., Wilkinson & Evans 1999; Sakamoto et al. 2003; Xue et al. 2008; Kafle et al. 2014; Wang et al. 2015; Elias et al. 2018), and the resulting range is less critical in our analysis.”
BackgroundConstraining the Milky Way mass with hypervelocity stars
Fragione, G., & Loeb, A. (2017) · New Astronomy · doi:10.1016/j.newast.2017.03.002 · Cited by 47
Bose, S., Deason, A. J., Belokurov, V. A., & Frenk, C. S. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1199 · Cited by 44
“Here we compare the average satellite luminosity function of Milky Way-mass haloes (M200 = 1 − 1.3 × 1012 M ; Smith et al. 2007; Deason et al. 2012; Wang et al. 2015; Patel et al. 2018; Callingham et al. 2019; Deason et al. 2019; Grand et al. 2019) with and without the inclusion of orphans.”
MethodInfluentialSelf-citationJoint constraints on the Galactic dark matter halo and GC from hypervelocity stars
Rossi, E. M., Marchetti, T., Cacciato, M., Kuiack, M., & Sari, R. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx098 · Cited by 50
“1 in Wang et al. 2015, and references therein).”
BackgroundBird, 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
Dark Matter in γ lines: Galactic Center vs. dwarf galaxies
Lefranc, V., Moulin, E., Paolo Panci, A., Sala, F., & Silk, J. I. (2016) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2016/09/043 · Cited by 41
How to suppress exponential growth—on the parametric resonance of photons in an axion background
Arza, A., Schwetz, T., & Todarello, E. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/10/013 · Cited by 41
“The potential, its derivative, and the growth factor σ are calculated at each location according to a typical NFW profile for the dark matter, taken from [47].”
BackgroundMethodThe mass profile of the Milky Way to the virial radius from the Illustris simulation
Taylor, C., Boylan-Kolchin, M., Torrey, P., Vogelsberger, M., & Hernquist, L. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1522 · Cited by 39
“Cosmological hydrodynamic simulations of individual MW-mass haloes have also been used to calibrate kinematic analyses of tracer populations in order to measure the mass of the MW (Xue et al. 2008; Rashkov et al. 2013; Piffl et al. 2014; Wang et al. 2015).”
MethodEvolution of LMC/M33-mass dwarf galaxies in the eagle simulation
Shao, S., Cautun, M., Deason, A. J., Frenk, C. S., & Theuns, T. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1470 · Cited by 40
“We further select a subset of LMC-mass satellites that reside in MW-mass haloes, which we define as any host halo with a mass in the range, M200 ∈ [0.5, 2] × 10 12 M⊙ (Cautun et al. 2014; Wang et al. 2015; Peñarrubia et al. 2016).”
BackgroundInfluentialSelf-citationThe history of the dark and luminous side of Milky Way-like progenitors
Graziani, L., de Bennassuti, M., Schneider, R., Kawata, D., & Salvadori, S. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx900 · Cited by 42
“Finally note the additional agreement with the gold filled circle, showing estimates of Wang et al. (2015), obtained by using dynamical tracers.”
BackgroundKoch, A., Grebel, E. K., & Martell, S. L. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201834825/pdf · Cited by 44
The tangential velocity excess of the Milky Way satellites
Cautun, M., & Frenk, C. S. (2017) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slx025 · Cited by 36
“Our results are insensitive to the host halo mass, so we use a broad mass range motivated by the large uncertainties in the MW halo mass (Wang et al. 2015) and the advantages of having a large sample of MW analogues.”
BackgroundMethodSelf-citationTHE PROPER MOTION OF PALOMAR 5
Fritz, T. K., & Kallivayalil, N. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/811/2/123 · Cited by 32
“Gibbons et al. (2014) obtain a value of 6× 1011 M⊙ using the Sgr stream, nearly a factor of three less than the mass obtained by Boylan-Kolchin et al. (2013): 16×1011 M⊙ using Leo I; see Wang et al. (2015) for a recent compilation of Milky Way mass measurements.”
MethodEadie, G. M., Springford, A., & Harris, W. E. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/835/2/167 · Cited by 37
“Despite the simplicity of the model, the results were in agreement with many other studies (see Wang et al. 2015, for a comparison figure). eadiegm@mcmaster.ca The promising results of Paper I led us to implement an arguably more realistic model for the Milky Way in Paper II, in which the…”
ResultThe Milky Way system in Λ cold dark matter cosmological simulations
Guo, Q., Cooper, A. P., Frenk, C. S., Helly, J. C., & Hellwing, W. A. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1938 · Cited by 34
“1 of Wang et al. 2015).”
ResultSelf-citationKapoor, A. U., Camps, P., Baes, M., Trc̆ka, A., Grand, R. J. J., van der Wel, A., Cortese, L., Looze, I. D., & Barrientos, D. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2043 · Cited by 34
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
“…van der Marel et al. 2012; Gibbons et al. 2014) and in general need a substantial degree of modelling and theory to be inferred (see e.g. Peebles et al. 2001; Li & White 2008; McMillan 2011; Fardal et al. 2013; Boylan-Kolchin et al. 2013; Diaz et al. 2014; Cautun et al. 2014; Wang et al. 2015).”
BackgroundLoebman, S., Valluri, M., Hattori, K., Debattista, V. P., Bell, E. F., Stinson, G., Christensen, C., Brooks, A. M., Quinn, T. R., & Governato, F. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa0d6 · Cited by 33
“The limitation of the line-of-sight velocities in recovering the velocity anisotropy was first explored in Hattori et al. (2013) and is supported by Wang et al. (2015), who find that if proper motions are not available, it is difficult to obtain robust constraints on β.”
BackgroundSTELLAR VELOCITY DISPERSION AND ANISOTROPY OF THE MILKY WAY INNER HALO
King, C., Brown, W. R., Geller, M. J., & Kenyon, S. J. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/813/2/89 · Cited by 34
“Recent simulations by Wang et al. (2015) evaluate potential biases in estimating the mass of the Milky Way using dynamical tracers.”
MethodThe galaxy size to halo spin relation of disc galaxies in cosmological hydrodynamical simulations
Yang, H., Gao, L., Frenk, C. S., Grand, R. J. J., Guo, Q., Liao, S., & Shao, S. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3335 · Cited by 31
“Here we follow (e.g. Wang et al. 2015a, 2020) to define Milky way sized galaxies as the galaxies whose halo masses are in the range,M200 ∈ [0.5, 2] × 1012 M , and dwarfs as those with halo masses ranging fromM200≤1.5×1011 M .”
BackgroundMethodInfluentialSelf-citationOn measuring the Galactic dark matter halo with hypervelocity stars
Contigiani, O., Rossi, E. M., & Marchetti, T. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1547 · Cited by 32
“As observed before in Wang et al. (2015), this is a perfect example of how assumptions, like imposing a massconcentration relation, can affect the results obtained with dynamical tracers.”
BackgroundResultProspects for finding sterile neutrino dark matter at KATRIN
Benso, C., Brdar, V., Lindner, M., & Werner Rodejohann, B. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.100.115035 · Cited by 28
“Such mass may be regarded as an upper value, given the multitude of previous measurements [59]; let us note that recent Gaia results seem to indicate a somewhat smaller Milky Way mass, but that measurement currently has large uncertainties [60].”
ResultThe orbital PDF: general inference of the gravitational potential from steady-state tracers
Han, J., Wang, W., Cole, S., & Frenk, C. S. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2707 · Cited by 28
“In Wilkinson & Evans (1999) and Wang et al. (2015), solutions of the form f(E,L) = f(E)L−2β were used to constrain the potential of the Galactic halo, where E and L are the energy and angular momentum of tracer particles.”
BackgroundMethodInfluentialSelf-citationWhat to expect from dynamical modelling of galactic haloes – II. The spherical Jeans equation
Wang, W., Han, J., Cole, S., More, S., Frenk, C. S., & Schaller, M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty706 · Cited by 27
“While we have thoroughly studied how well the potential profile can be recovered from different dynamical models in a series of previous studies (Wang et al. 2015; Han et al. 2016a,b; Wang et al. 2017), in this work we focus on presenting results on the recovered virial mass and concentration…”
BackgroundMethodInfluentialSelf-citationDetermination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies
Li, Z.-Z., Jing, Y. P., Qian, Y.-Z., Yuan, Z., & Zhao, D.-H. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa94c0 · Cited by 30
“Various methods have been proposed to measure this important quantity (see Courteau et al. 2014; Bland-Hawthorn & Gerhard 2016 for reviews and Wang et al. 2015 for a comparison of recent measurements).”
MethodThe effect of tides on the Sculptor dwarf spheroidal galaxy
Iorio, G., Nipoti, C., Battaglia, G., & Sollima, A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1342 · Cited by 24
“5) assuming the c200-M200 relation at z = 0.8 (Diemer & Joyce 2019).”
MethodResultInfluentialHan, J., Wang, W., Cole, S., & Frenk, C. S. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2522 · Cited by 25
“Note that stars with low binding energies are also those that have been accreted recently (Wang et al. 2015).”
BackgroundMethodResultInfluentialSelf-citationTHE CONNECTION BETWEEN THE HOST HALO AND THE SATELLITE GALAXIES OF THE MILKY WAY
Lu, Y., Benson, A., Mao, Y.-Y., Tonnesen, S. K., Peter, A. H. G., Wetzel, A. R., Boylan-Kolchin, M., & Wechsler, R. H. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/830/2/59 · Cited by 25
“In recent studies, Wang et al. (2015) found that halo concentration strongly affects the estimate of halo mass using dynamical tracers of the MW. Mao et al. (2015) demonstrated that halo concentration influences the inferences for the mass and other properties of the MW halo from satellite…”
BackgroundLi, Q., Han, J., Wang, W., Cui, W., Luca, F. D., Yang, X., Zhou, Y., & Shi, R. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1739 · Cited by 24
Self-citationThe energy distribution of the first supernovae
Koutsouridou, I., Salvadori, S., Skúladóttir, Á., Rossi, M., Vanni, I., & Pagnini, G. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2304 · Cited by 34
Galaxy Formation in Sterile Neutrino Dark Matter Models
Menci, N., Grazian, A., Lamastra, A., Calura, F., Castellano, M., & Santini, P. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa773 · Cited by 23
“…with DM mass in the range M = 1 − 2.5 · 1012 M (where M is the mass of a spherical volume with mean density equal to 200 times the critical density), which covers the bulk of the observational estimates of the Milky Way mass (for a comprehensive account of such measurements, see Wang et al. 2015).”
BackgroundInfluentialWhat galaxy masses perturb the local cosmic expansion?
Peñarrubia, J., & Fattahi, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx323 · Cited by 21
“Tests against mock data sets reveal that the uncertainty is largely dominated by (i) the unknown impact of baryons on the halo density profile and (ii) the unknown orbital distribution of the tracer particles (e.g. Wang et al. 2015).”
BackgroundEstimating the Milky Way's Mass via Hierarchical Bayes: A Blind Test on MUGS2 Simulated Galaxies
Eadie, G., Keller, B., & Harris, W. E. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aadb95 · Cited by 20
“The total mass of the Milky Way (MW) Galaxy is not known within a factor of two (see Figure 1 in Wang et al. 2015, for a dramatic illustration of M200 values).”
BackgroundWhat to expect from dynamical modelling of galactic haloes
Wang, W., Han, J., Cole, S., Frenk, C. S., & Sawala, T. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1334 · Cited by 20
“5 to 2.5 × 1012M⊙ (Wang et al. 2015).”
BackgroundMethodInfluentialSelf-citationZhang, D., Luo, Y., & Kang, X. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz957 · Cited by 19
“The comparsion of these two samples are shown in the bottom-right panel. concentrate at around 1012 M (Li et al. (2018); see Callingham et al. (2018) and Wang et al. (2015) for a summary of different methods and results).”
BackgroundTHE CONNECTION BETWEEN THE HOST HALO AND THE SATELLITE GALAXIES OF THE MILKY WAY
Lu, Y., Benson, A., Mao, Y.-Y., Tonnesen, S. K., Peter, A. H. G., Wetzel, A. R., Boylan-Kolchin, M., & Wechsler, R. H. (2016) · eScholarship (California Digital Library) · Cited by 17
Li, Q., Han, J., Wang, W., Cui, W., Li, Z., & Yang, X. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1633 · Cited by 18
Self-citationCooper, A. P., Cole, S., Frenk, C. S., Bret, T. L., & Pontzen, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx955 · Cited by 18
“1 of Wang et al. 2015).”
Self-citationPush it to the limit: Local Group constraints on high-redshift stellar mass functions forM⋆≥ 105 M⊙
Graus, A. S., Bullock, J. S., Boylan-Kolchin, M., & Weisz, D. R. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2728 · Cited by 17
“This spans the range of most recent measurements but there are some estimates that fall as low as 7 × 1011 M (see, e.g. Boylan-Kolchin et al. 2013; Wang et al. 2015).”
BackgroundOn the impact of neutron star binaries’ natal-kick distribution on the Galactic r-process enrichment
Safarzadeh, M., & Côté, B. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1897 · Cited by 17
“We consider a MW-like dark matter halo with a current mass of 1012 M (Wang et al. 2015).”
BackgroundHe, J., Wang, W., Li, Z., Han, J., Rodríguez-Gómez, V., Zhao, D., Meng, X. T., Jing, Y., Shao, S., Shi, R., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8882 · Cited by 16
Self-citationLi, Z., Qian, Y.-Z., Han, J., Wang, W., & Jing, Y. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab4f6d · Cited by 15
“As shown by Wang et al. (2015) and Han et al. (2016b), introducing unjustified assumptions into the construction of the DF may lead to substantially biased results.”
BackgroundSelf-citationStructure formation limits on axion-like dark matter
Baumholzer, S., Brdar, V., & Morgante, E. (2021) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2021/05/004 · Cited by 15
“5 × 1012M (see [53–57] and references therein), using recent data from the GAIA survey.”
MethodNo certainty of a Milky Way–Andromeda collision
Sawala, T., Delhomelle, J., Deason, A. J., Frenk, C. S., Häkkinen, J., Johansson, P. H., Keitaanranta, A., Rawlings, A., & Wright, R. J. (2025) · Nature Astronomy · doi:10.1038/s41550-025-02563-1 · Cited by 15
“The initial masses, concentrations, positions and velocities were chosen from among the same sample of fiducial systems shown in Figs.”
Self-citationLocal Group Analogs in ΛCDM Cosmological Simulations
Zhai, M., Guo, Q., Zhao, G., Gu, Q., & Liu, A. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab6986 · Cited by 13
“It is usually estimated using kinematics of the satellite galaxies and halo stars (e.g. Wilkinson & Evans 1999; Sakamoto et al. 2003; Xue et al. 2008; Wang et al. 2015; Zhai et al. 2018).”
MethodResultDynamical response of dark matter to galaxy evolution affects direct-detection experiments
Petersen, M. S., Katz, N. S., & Weinberg, M. D. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.94.123013 · Cited by 12
Is The Vast Polar Structure Of Dwarf Galaxies A Serious Problem For ΛCDM?
Lipnicky, A., & Chakrabarti, S. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx286 · Cited by 12
“1 of Wang et al. 2015).”
Cosmic transients, Einstein’s Equivalence Principle and dark matter halos
Orfeu Bertolami, A., & Landim, R. G. (2018) · Physics of the Dark Universe · doi:10.1016/j.dark.2018.05.002 · Cited by 11
“[44], the NFW potential is found from Eq.”
BackgroundMethodResultWang, W., Ling, Z., Li, Z., Chen, Y., Han, J., He, F., Yang, X., Jing, Y., Frenk, C. S., Nie, J., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9b19 · Cited by 12
“This is in good agreement with the commonly accepted experience that the mass enclosed within the half-mass (or half-light) radius of tracers can be more robustly constrained upon dynamical modeling (e.g. Wolf et al. 2010; Walker & Peñarrubia 2011; Wang et al. 2015, 2020).”
ResultSelf-citationNon-parametric spherical Jeans mass estimation with B-splines
Rehemtulla, N., Valluri, M., & Vasiliev, E. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac400 · Cited by 13
Jeans that fit: weighing the mass of the Milky Way analogues in the ΛCDM universe
Kafle, P. R., Sharma, S., Robotham, A. S. G., Elahi, P. J., & Driver, S. P. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty118 · Cited by 12
“Similarly, Wang et al. (2015) test the accuracy of a phase-space distribution function in measuring the mass of the MW dark matter halo.”
BackgroundMethodemPDF : inferring the Milky Way mass with data-driven distribution function in phase space
Li, Z., Han, J., Wang, W., Qian, Y.-Z., Li, Q., Jing, Y., & Li, T. S. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf358 · Cited by 15
Self-citationUnraveling the Complexity of Dwarf Galaxy Dynamics: A Study of Binary Orbital Motions
Wang, W., Ling, Z., Jing, Y., Grand, R. J. J., Li, Z., Fu, X., Li, L., Han, J., Li, T. S., Feng, F., et al. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acf314 · Cited by 9
“The virial masses 15 of their host dark matter halos are in the range of 1 – 2 × 10 12 M e , to represent the virial mass of our MW ( e.g., Wang et al. 2020, 2015 ) .”
BackgroundSelf-citationShi, R., Wang, W., Li, Z., Han, J., Shi, J., Rodríguez-Gómez, V., Peng, Y., & Li, Q. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1541 · Cited by 9
Self-citationThe abundance of satellite galaxies in the inner region of ΛCDM Milky Way sized haloes
Li, M., Gao, L., & Wang, J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3292 · Cited by 8
JEANS ANALYSIS OF THE GALACTIC THICK DISK AND THE LOCAL DARK MATTER DENSITY
Sánchez-Salcedo, F. J., Flynn, C., & de Diego, J. A. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/817/1/13 · Cited by 8
“It is now generally accepted that our Galaxy contains a dark matter (DM) halo with a virial mass between 0.6×1012M⊙ and 3×1012M⊙ (e.g., Wang et al. 2015 and references therein).”
BackgroundInfluential
Metadata
- Authors
- Wang, W., Han, J., Cooper, A. P., Cole, S., Frenk, C., & Lowing, B.
- Affiliations
- Durham University (GB)
- Corresponding author
- Wang, Wenting
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2015-08-13
- Volume
- 453
- Issue
- 1
- Pages
- 377-400
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W1883919649
- Cited by
- 116
- References
- 95
- Citations by year
- 2026: 1 · 2025: 5 · 2024: 3 · 2023: 3 · 2022: 7 · 2021: 6 · 2020: 10 · 2019: 14 · 2018: 18 · 2017: 19 · 2016: 21 · 2015: 9
- FWCI
- 12.44
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Durham Research Online (Durham University) (publishedVersion, other-oa)
- Durham Research Online (Durham University) (acceptedVersion)
- arXiv (Cornell University) (submittedVersion)
- Durham Research Online (Durham University) (submittedVersion, cc-by)
- HighWire Press Open Archive (submittedVersion)
- arXiv (Cornell University)
- Funders
- Durham University (ST/K00042X/1, ST/K003267/1, ST/H008519/1)
- Rijksuniversiteit Groningen
- Science and Technology Facilities Council (ST/I00162X/1, ST/H008519, ST/K00042X/1, ST/M007006/1, ST/L00075X/1, ST/H008519/1, ST/K003267/1)
- Leibniz-Gemeinschaft
- 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 › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- Milky Way dark matter halo, halo mass estimation, stellar halo, Navarro-Frenk-White profile, halo concentration, mass bias, velocity anisotropy, dynamic equilibrium, Aquarius simulations, maximum likelihood fitting
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