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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
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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
Equation of State Calculations by Fast Computing Machines
Metropolis, N., Rosenbluth, A. W., Rosenbluth, M. N., Teller, A. H., & Teller, E. (1953) · The Journal of Chemical Physics · doi:10.1063/1.1699114 · Cited by 37,192
Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. (2013) · Publications of the Astronomical Society of the Pacific · doi:10.1086/670067 · Cited by 14,336 · cited 1×
“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
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · The Astrophysical Journal · doi:10.1086/177173 · Cited by 8,544
Prusti, T., de Bruijne, J. H. J., Brown, A. G. A., Vallenari, A., Babusiaux, C., Bailer‐Jones, C. A. L., Bastian, U., Biermann, M., Evans, D. W., Eyer, L., et al. (2016) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201629272 · Cited by 7,350
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×
“…‘hole’ in the stellar density for the same reasons given in Paper I. TheJurić et al.(2008) analysis of data from the Sloan Digital Sky Survey (SDSS:Abazajian et al. 2009) showed that the approximation to exponential profiles is a sensible one for the Milky Way, and produced estimates based on…”
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).”
BackgroundMethodInfluentialMONITORING STELLAR ORBITS AROUND THE MASSIVE BLACK HOLE IN THE GALACTIC CENTER
Gillessen, S., Eisenhauer, F., Trippe, S., Alexander, T., Genzel, R., Martins, F., & Ott, T. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/692/2/1075 · Cited by 1,779 · cited 1×
“Nonetheless, we also consider the case with a weaker prior on R0, specifically the prior that we took in Paper I, which is simply derived from the measurements of the orbits of stars around Sgr A* by Gillessen et al.(2009), and isR0 = 8.33 ± 0.35 kpc.”
ResultInfluentialThe Galaxy in Context: Structural, Kinematic, and Integrated Properties
Bland-Hawthorn, J., & Gerhard, O. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081915-023441 · Cited by 1,656 · cited 17×
“The recent estimate ofR0 ∼ 7.9 kpc from a new reduction of observations showing the orbits of stars around Sgr A* (Boehle et al. 2016) would appear to cast fresh uncertainty on this value when it seemed as if most estimates were tendingtowards∼8.2− 8.3 kpc (Bland-Hawthorn & Gerhard 2016).”
BackgroundResultInfluentialGalactic star formation and accretion histories from matching galaxies to dark matter haloes
Moster, B. P., Naab, T., & White, S. D. M. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts261 · Cited by 1,431 · cited 1×
“Moster et al.(2013) assume an intrinsic scatter around this relationship of 0.15 in log10 M∗, and also give a ‘plausible range’ for all of the parameters in equation7.”
BackgroundInfluentialReid, M. J., Menten, K. M., Brunthaler, A., Zheng, X. W., Dame, T. M., Xu, Y., Wu, Y., Zhang, B., Sanna, A., Sato, M., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/783/2/130 · Cited by 1,379 · cited 4×
“This represents an increase by more than a fctor of 4 over the number of HMSFRs with known parallaxes used in Paper I.Reid et al.(2014) used these data to determine the Sun’s position and velocity with aχ2 analysis which used the approximation that the HMSFRs were exactly at the position…”
BackgroundMethodInfluentialThe Milky Way Tomography with SDSS. I. Stellar Number Density Distribution
Jurić, M., Ivezić, Ž., Brooks, A. M., Lupton, R. H., Schlegel, D. J., Finkbeiner, D. P., Padmanabhan, N., Bond, N., Sesar, B., Rockosi, C. M., et al. (2008) · The Astrophysical Journal · doi:10.1086/523619 · Cited by 1,318
Ground-based and Airborne Instrumentation for Astronomy
McLean, I. S., & Iye, M. (2006) · Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series · Cited by 1,201
SEGUE: A SPECTROSCOPIC SURVEY OF 240,000 STARS WITH g = 14-20
Yanny, B., Rockosi, C., Newberg, H. J., Knapp, G. R., Adelman-McCarthy, J. K., Alcorn, B., Allam, S., Prieto, C. A., An, D., Anderson, K. S. J., et al. (2009) · The Astronomical Journal · doi:10.1088/0004-6256/137/5/4377 · Cited by 1,162 · cited 1×
“…used similar constraints from maser sources to those used in this study), andBovy & Rix (2013) who fit quasi-isothermal distribution functions (Binney & McMillan 2011) to ‘mono-abundance populations’ (groups of stars in a small range of [Fe/H] and [α/Fe]) from the SEGUE survey (Yanny et al. 2009).”
MethodLocal stellar kinematics from Hipparcos data
Dehnen, W., & Binney, J. J. (1998) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1998.01600.x · Cited by 1,049
Gilmore, G., & Reid, N. (1983) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/202.4.1025 · Cited by 990 · cited 1×
“The Milky Way’s stellar disc is commonly decomposed into a thin and thick disc (e.g.Gilmore & Reid 1983).”
BackgroundResolving cosmic structure formation with the Millennium-II Simulation
Boylan-Kolchin, M., Springel, V., White, S. D. M., Jenkins, A., & Lemson, G. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15191.x · Cited by 912 · 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).”
MethodLocal stellar kinematics from hipparcos dataPreprint
Dehnen, W., & Binney, J. J. (1998) · Cited by 828
Reid, M., Menten, K., Zheng, X.-W., Brunthaler, A., Moscadelli, L., Xu, Y., Zhang, B., Sato, M., Honma, M., Hirota, T., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/700/1/137 · Cited by 799 · cited 4×
“They have therefore been used by numerous authors to constrain the properties of the Milky Way (e.g.,Reid et al. 2009a; McMillan & Binney 2010; Bovy et al. 2009; Bobylev & Bajkova 2013; Reid et al. 2014, Paper I).”
MethodInfluentialThe Proper Motion of Sagittarius A*. II. The Mass of Sagittarius A*
Reid, M. J., & Brunthaler, A. (2004) · The Astrophysical Journal · doi:10.1086/424960 · Cited by 791
McMillan, P. J. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18564.x · Cited by 789 · cited 2×
“…used similar constraints from maser sources to those used in this study), andBovy & Rix (2013) who fit quasi-isothermal distribution functions (Binney & McMillan 2011) to ‘mono-abundance populations’ (groups of stars in a small range of [Fe/H] and [α/Fe]) from the SEGUE survey (Yanny et al. 2009).”
BackgroundMethodSelf-citationXue, X.-X., Rix, H., Zhao, G., Fiorentin, P. R., Naab, T., Steinmetz, M., van den Bosch, F. C., Beers, T. C., Lee, Y. S., Bell, E. F., et al. (2008) · The Astrophysical Journal · doi:10.1086/589500 · Cited by 716 · cited 1×
“Deason et al.(2012) and Xue et al. (2008) used samples of blue horizontal branch stars to determine the mass contained within 50 and 60 kpc (respectively).”
MethodΛCDM‐based Models for the Milky Way and M31. I. Dynamical Models
Klypin, A. A., Zhao, H., & Somerville, R. S. (2002) · The Astrophysical Journal · doi:10.1086/340656 · Cited by 692
Governato, F., Zolotov, A., Pontzen, A., Christensen, C., Oh, S.-H., Brooks, A. M., Quinn, T., Shen, S., & Wadsley, J. W. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20696.x · Cited by 652 · cited 1×
“…influence will be at the centre, but whether, for Milky Way sized galaxies, this influence will beto steepen the inner density ‘cusp’ (corresponding toγ > 1 in eq.5) or to weaken it, producing more of a ‘core’ (γ < 1) is an active area of research (e.g.Duffy et al. 2010; Governato et al. 2012).”
BackgroundThe RAVE survey: constraining the local Galactic escape speed
Smith, M. C., Ruchti, G. R., Helmi, A., Wyse, R. F. Ġ., Fulbright, J. P., Freeman, K. C., Navarro, J. F., Seabroke, G. M., Steinmetz, M., Williams, M., et al. (2007) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2007.11964.x · Cited by 629
Reid, M. J., Menten, K. M., Brunthaler, A., Zheng, X., Dame, T. M., Xu, Y., Wu, Y., Zhang, B., Sanna, A., Sato, M., et al. (2014) · Cited by 629
A novel determination of the local dark matter density
Catena, R., & Ullio, P. (2010) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2010/08/004 · Cited by 625 · cited 1×
“3), including Paper I,Catena & Ullio (2010), and Nesti & Salucci(2013).”
BackgroundThe shape of dark matter haloes: dependence on mass, redshift, radius and formation
Allgood, B., Flores, R. A., Primack, J. R., Kravtsov, A. V., Wechsler, R. H., Faltenbacher, A., & Bullock, J. S. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10094.x · Cited by 588 · cited 1×
“1 we explore the effect of varying the assumed value of γ. MNRAS 000, 1–19 (2016) Haloes in dark-matter-only cosmological simulations tend to be significantly prolate, but with a great deal of variation in axis ratios (e.g.Allgood et al. 2006).”
BackgroundResolving Cosmic Structure Formation with the Millennium-II SimulationPreprint
Boylan-Kolchin, M., Springel, V., White, S. D. M., Jenkins, A. R., & Lemson, G. (2009) · Cited by 571
THE SAGITTARIUS DWARF GALAXY: A MODEL FOR EVOLUTION IN A TRIAXIAL MILKY WAY HALO
Law, D. R., & Majewski, S. R. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/714/1/229 · Cited by 550 · cited 1×
“Famously, models of the Sagittarius stream have been used to argue that the dark-matter halo is oblate (e.g. Johnston, Law & Majewski 2005), prolateHelmi (2004) or triaxial (Law & Majewski 2010, though this is effectively oblate with the short axis in the plane of the Galaxy).”
MethodBovy, J., & Rix, H.-W. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/779/2/115 · Cited by 523 · cited 1×
“It also provides a helpful estimate of the potential that can be refined by dynamical modelling (e.g.McMillan & Binney 2013; Bovy & Rix 2013; Piffl et al. 2014a).”
BackgroundThe Local Dark Matter DensityPreprint
Read, J. I. (2016) · Cited by 494
Read, J. I. (2014) · Journal of Physics G: Nuclear and Particle Physics · doi:10.1088/0954-3899/41/6/063101 · Cited by 489 · cited 3×
“In the Solar neighbourhood,Read(2014) noted that the comparison of constraints from the rotation curve (which providesan estimate of the spherically averaged enclosed dark-matter content) and estimates of the local density provide a constraint on the halo shape which is consistent with spherical or…”
BackgroundInfluentialTHE SPATIAL STRUCTURE OF MONO-ABUNDANCE SUB-POPULATIONS OF THE MILKY WAY DISK
Bovy, J., Rix, H., Liu, C., Hogg, D. W., Beers, T. C., & Lee, Y. S. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/753/2/148 · Cited by 445 · cited 4×
“These arguments still hold, and suggest that both theSchönrich(2012) and Bovy et al.(2012b) results should be treated with some scepticism.”
BackgroundResultInfluentialDehnen, W., & Binney, J. J. (1998) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1998.01282.x · Cited by 438
THE MILKY WAY'S CIRCULAR-VELOCITY CURVE BETWEEN 4 AND 14 kpc FROM APOGEE DATA
Bovy, J., Allende Prieto, C., Beers, T. C., Bizyaev, D., da Costa, L. N., Cunha, K., Ebelke, G. L., Eisenstein, D. J., Frinchaboy, P. M., García Pérez, A. E., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/759/2/131 · Cited by 413 · cited 4×
“These arguments still hold, and suggest that both theSchönrich(2012) and Bovy et al.(2012b) results should be treated with some scepticism.”
BackgroundResultInfluentialThe distribution of stellar mass in the low-redshift Universe
Li, C., & White, S. D. M. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15268.x · Cited by 393
The present and future mass of the Milky Way halo
Wilkinson, M. I., & Evans, N. W. (1999) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1999.02964.x · Cited by 383
THE RADIAL VELOCITY EXPERIMENT (RAVE): FOURTH DATA RELEASE
Kordopatis, G., Gilmore, G. F., Steinmetz, M., Boeche, C., Seabroke, G. M., Siebert, A., Zwitter, T., Binney, J. J., de Laverny, P., Recio-Blanco, A., et al. (2013) · The Astronomical Journal · doi:10.1088/0004-6256/146/5/134 · Cited by 378
Self-citationPortail, M., Gerhard, O., Wegg, C., & Ness, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2819 · Cited by 378
The masses of the Milky Way and Andromeda galaxies
Watkins, L. L., Evans, N. W., & An, J. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16708.x · Cited by 365 · cited 1×
“Watkins et al.(2010) used a sample of 26 satellite galaxies (including six with proper motions) to find the mass of the Milky Way within 300 kpc, and found that the answer depended sensitively on the assumed velocity anisotropy of the satellites, with a mass estimate that was (1.4 ± 0.3) × 1012 M⊙…”
MethodInfluentialDehnen, W., & Binney, J. J. (1998) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-8711.1998.01282.x · Cited by 363
AN IMPROVED DISTANCE AND MASS ESTIMATE FOR SGR A* FROM A MULTISTAR ORBIT ANALYSIS
Boehle, A., Ghez, A. M., Schödel, R., Meyer, L., Yelda, S., Albers, S., Martinez, G. D., Becklin, E. E., Do, T., Lu, J. R., et al. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/830/1/17 · Cited by 349 · cited 2×
“…interest, however, that a more recent analysis of the astrometry of faint stars orbiting Sgr A*, combining two different types of imaging over a time baseline of two decades finds a lower value ofR0 = (7.86±0.14±0.04) kpc (statistical and systematic uncertainties respectively,Boehle et al. 2016).”
BackgroundResultInfluentialThe photometric structure of the inner Galaxy
Binney, J. J., Gerhard, O., & Spergel, D. N. (1997) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/288.2.365 · Cited by 346 · cited 1×
“So, to find the properties of the Sun’s orbit, takingR0 and v0 from Table2, z0 from Binney et al.(1997) and the Solar peculiar velocity fromSchönrich et al.(2010), one would run ./findOrbitProperties.exe 8.2 0.014 11.1 7.25 -245 and receive the output Guiding Centre radius: 8.62121 Minimum,…”
BackgroundInfluentialThe Dark Matter halo of the Milky Way, AD 2013
Nesti, F., & Salucci, P. (2013) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2013/07/016 · Cited by 341 · cited 1×
“3), including Paper I,Catena & Ullio (2010), and Nesti & Salucci(2013).”
BackgroundStructural Parameters of Thin and Thick Disks in Edge-on Disk Galaxies
Yoachim, P., & Dalcanton, J. J. (2006) · The Astronomical Journal · doi:10.1086/497970 · Cited by 337 · cited 1×
“Since the high [α/Fe] component also has a larger scale height than the low [α/Fe] population, this might appear to be in conflict with the Jurić et al.(2008) result, and with thick discs observed in external galaxies (e.g.Yoachim & Dalcanton 2006), where the thick disc has the longer scale length.”
ResultThe RAVE survey: the Galactic escape speed and the mass of the Milky Way
Piffl, T., Scannapieco, C., Binney, J. J., Steinmetz, M., Scholz, R. ‐., Williams, M. E. K., de Jong, R. S., Kordopatis, G., Matijevič, G., Bienaymé, O., et al. (2013) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201322531 · Cited by 333 · cited 4×
“Piffl et al.(2014a) also noted that the axis ratio of the dark-matter halo has an important influence on the derived local density when interpreting dynamical models of the disc, withρh,⊙ ∝ q−0.89.”
BackgroundResultInfluentialGalactic rotation and solar motion from stellar kinematics
Schönrich, R. A. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21631.x · Cited by 306 · cited 2×
“Schönrich(2012) suggested thatSchönrich et al.(2010) may have underestimated the value ofU⊙, and that it may be∼14 km s−1.”
BackgroundInfluentialTWO RED CLUMPS AND THE X-SHAPED MILKY WAY BULGE
McWilliam, A., & Zoccali, M. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/724/2/1491 · Cited by 299 · cited 1×
“It is increasingly clear that it is a boxy (or ‘peanut shaped’) bulge (McWilliam & Zoccali 2010; Nataf et al. 2010; Ness et al. 2012, and others).”
BackgroundThe mass distribution within our Galaxy - A three component model
Caldwell, J. A. R., & Ostriker, J. P. (1981) · The Astrophysical Journal · doi:10.1086/159441 · Cited by 291 · cited 1×
“A famous early example was that of Schmidt(1956), with further examples being provided by Caldwell & Ostriker(1981), Dehnen & Binney(1998a, henceforth DB98), Klypin, Zhao & Somerville(2002) and the previous paper in this series (McMillan 2011, henceforth Paper I).”
BackgroundThe galactic disk surface mass density and the Galactic force K(z) at Z = 1.1 kiloparsecs
Kuijken, K., & Gilmore, G. (1991) · The Astrophysical Journal · doi:10.1086/185920 · Cited by 286
Spiral arms, bar shape and bulge microlensing in the Milky Way
Bissantz, N., & Gerhard, O. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2002.05116.x · Cited by 262
AN IMPROVED DISTANCE AND MASS ESTIMATE FOR SGR A* FROM A MULTISTAR ORBIT ANALYSIS
Boehle, A., Ghez, A., Schödel, R., Meyer, L., Yelda, S., Albers, S. M., Martinez, G. D., Becklin, E., Do, T., Lu, Jr., et al. (2016) · eScholarship (California Digital Library) · Cited by 251
THE SPLIT RED CLUMP OF THE GALACTIC BULGE FROM OGLE-III
Nataf, D. M., Udalski, A., Gould, A. P., Fouqué, P., & Stanek, K. Z. (2010) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/721/1/l28 · Cited by 249 · cited 1×
“It is increasingly clear that it is a boxy (or ‘peanut shaped’) bulge (McWilliam & Zoccali 2010; Nataf et al. 2010; Ness et al. 2012, and others).”
BackgroundThe distribution of stellar mass in the low-redshift UniversePreprint
Li, C., & White, S. D. M. (2009) · Cited by 245
Global properties of the H I distribution in the outer Milky Way
Kalberla, P. M. W., & Dedes, L. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20079240 · Cited by 244
‘Skinny Milky Way please’, says Sagittarius
Gibbons, S. L. J., Belokurov, V. A., & Evans, N. W. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1986 · Cited by 242
A TRIGONOMETRIC PARALLAX OF Sgr B2
Reid, M. J., Menten, K. M., Zheng, X., Brunthaler, A., & Xu, Y. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/705/2/1548 · Cited by 239 · cited 4×
“They have therefore been used by numerous authors to constrain the properties of the Milky Way (e.g.,Reid et al. 2009a; McMillan & Binney 2010; Bovy et al. 2009; Bobylev & Bajkova 2013; Reid et al. 2014, Paper I).”
MethodInfluentialJohnston, K. V., Law, D. R., & Majewski, S. R. (2005) · The Astrophysical Journal · doi:10.1086/426777 · Cited by 237 · cited 1×
“The study of the Sagittarius stream by Johnston et al.(2005) had best fitting models with masses in the range (3.8− 5.6)× 1011 within 50 kpc, which is in keeping with our prior.”
ResultInfluentialThere's no place like home? Statistics of Milky Way-mass dark matter haloes
Boylan-Kolchin, M., Springel, V., White, S. D. M., & Jenkins, A. R. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16774.x · Cited by 228 · cited 1×
“We take a prior on concentration, cv′ , from Boylan-Kolchin et al. (2010)4 who found that, for the mass range that the Milky Way’s halo is very likely to lie in, the 4 There are varying definitions of the virial radius, and in this case the definition is the radius of a sphere with average density…”
BackgroundGLOBULAR CLUSTER STREAMS AS GALACTIC HIGH-PRECISION SCALES—THE POSTER CHILD PALOMAR 5
Küpper, A. H. W., Balbinot, E., Bonaca, A., Johnston, K. V., Hogg, D. W., Kroupa, P., & Santiago, B. X. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/803/2/80 · Cited by 228 · cited 1×
“Küpper et al.(2015) used the position of apparent overdensities in the tidal tails of Palomar 5 to determine the mass within its apogalactic radius.”
MethodVelocity Trends in the Debris of Sagittarius and the Shape of the Dark Matter Halo of Our Galaxy
Helmi, A. (2004) · The Astrophysical Journal · doi:10.1086/423340 · Cited by 225
Duffy, A. R., Schaye, J., Kay, S. T., Dalla Vecchia, C., Battye, R. A., & Booth, C. M. (2010) · MPG.PuRe (Max Planck Society) · Cited by 220
Bensby, T., Alves-Brito, A., Oey, M. S., Yong, D., & Meléndez, J. (2011) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/735/2/l46 · Cited by 218
ON THE SHOULDERS OF GIANTS: PROPERTIES OF THE STELLAR HALO AND THE MILKY WAY MASS DISTRIBUTION
Kafle, P. R., Sharma, S., Lewis, G. F., & Bland-Hawthorn, J. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/794/1/59 · Cited by 215 · cited 1×
“Kafle et al.(2014) use similar techniques to this paper (and Paper I) to determine a best fitting mass model for the Milky Way as a whole, taking into account many constraints.”
MethodGas dynamics in the Milky Way: second pattern speed and large-scale morphology
Bissantz, N., Englmaier, P., & Gerhard, O. (2003) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2003.06358.x · Cited by 213
Chemodynamics of the Milky Way
Anders, F., Chiappini, C., Santiago, B. X., Rocha–Pinto, H. J., Girardi, L., da Costa, L. N., Maia, M. A. G., Steinmetz, M., Minchev, I., Schultheis, M., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201323038 · Cited by 212
The uncertainty in Galactic parameters
McMillan, P. J., & Binney, J. J. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15932.x · Cited by 204 · cited 4×
“They have therefore been used by numerous authors to constrain the properties of the Milky Way (e.g.,Reid et al. 2009a; McMillan & Binney 2010; Bovy et al. 2009; Bobylev & Bajkova 2013; Reid et al. 2014, Paper I).”
BackgroundMethodInfluentialSelf-citationChatzopoulos, S., Fritz, T. K., Gerhard, O., Gillessen, S., Wegg, C., Genzel, R., & Pfuhl, O. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2452 · Cited by 201 · cited 3×
“We take a constraint onR0 from Chatzopoulos et al.(2015).”
BackgroundMethodInfluentialON THE FORMATION OF GALACTIC THICK DISKS
Minchev, I., Martig, M., Streich, D., Scannapieco, C., de Jong, R. S., & Steinmetz, M. (2015) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/804/1/l9 · Cited by 199 · cited 1×
“However, this is simply becausether is a distinction between defining the thick disc chemically, and defining it morphologically, easily explained if the chemically-defined discs are flared (e.g.Minchev et al. 2015).”
BackgroundConstraining the Galaxy's dark halo with RAVE stars
Piffl, T., Binney, J. J., McMillan, P. J., Steinmetz, M., Helmi, A., Wyse, R. F. Ġ., Bienaymé, O., Bland‐Hawthorn, J., Freeman, K. C., Gibson, B. K., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1948 · Cited by 198 · cited 4×
“Piffl et al.(2014a) also noted that the axis ratio of the dark-matter halo has an important influence on the derived local density when interpreting dynamical models of the disc, withρh,⊙ ∝ q−0.89.”
BackgroundResultInfluentialSelf-citationThe Causes of Halo Shape Changes Induced by Cooling Baryons: Disks versus Substructures
Debattista, V. P., Moore, B., Quinn, T., Kazantzidis, S., Maas, R. W., Mayer, L., Read, J. I., & Stadel, J. (2008) · The Astrophysical Journal · doi:10.1086/587977 · Cited by 190 · cited 1×
“It is recognised that, again, baryonic physics will play an important role – condensationof baryons to the centres of haloes is expected to make them rounder than dark-matter-only simulations would suggest (Debattista et al. 2008).”
BackgroundDuffy, A. R., Schaye, J., Kay, S. T., Vecchia, C. D., Battye, R. A., & Booth, C. M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16613.x · Cited by 186 · cited 2×
“…influence will be at the centre, but whether, for Milky Way sized galaxies, this influence will beto steepen the inner density ‘cusp’ (corresponding toγ > 1 in eq.5) or to weaken it, producing more of a ‘core’ (γ < 1) is an active area of research (e.g.Duffy et al. 2010; Governato et al. 2012).”
BackgroundKinematics and chemical properties of the old disk of the Galaxy
Lewis, J. R., & Freeman, K. C. (1989) · The Astronomical Journal · doi:10.1086/114963 · Cited by 180
GALACTIC MASERS AND THE MILKY WAY CIRCULAR VELOCITY
Bovy, J., Hogg, D. W., & Rix, H. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/704/2/1704 · Cited by 178 · cited 2×
“They have therefore been used by numerous authors to constrain the properties of the Milky Way (e.g.,Reid et al. 2009a; McMillan & Binney 2010; Bovy et al. 2009; Bobylev & Bajkova 2013; Reid et al. 2014, Paper I).”
MethodTHE ORIGIN OF THE SPLIT RED CLUMP IN THE GALACTIC BULGE OF THE MILKY WAY
Ness, M., Freeman, K. C., Athanassoula, E., Boer, E. W.-D., Bland‐Hawthorn, J., Lewis, G. F., Yong, D., Asplund, M., Lane, R. R., Kiss, L. L., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/756/1/22 · Cited by 177 · cited 1×
“It is increasingly clear that it is a boxy (or ‘peanut shaped’) bulge (McWilliam & Zoccali 2010; Nataf et al. 2010; Ness et al. 2012, and others).”
BackgroundMade-to-measure models of the Galactic box/peanut bulge: stellar and total mass in the bulge region
Portail, M., Wegg, C., Gerhard, O., & Martínez-Valpuesta, I. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv058 · Cited by 175 · cited 4×
“Portail et al.(2015) used Made-To-Measure modelling to determine the mass within a box around the Galactic centre of a volume (±2.2 ± 1.4 ± 1.2) kpc, determining that it is (1.84 ± 0.07) × 1010 M⊙ (and the closely related study byPortail et al. 2016, found a very similar value – (1.85± 0.05)× 1010…”
BackgroundMethodResultInfluentialGalactic rotation and solar motion from stellar kinematics
Schönrich, R. A. (2012) · MPG.PuRe (Max Planck Society) · Cited by 168
EVIDENCE FOR A TRIAXIAL MILKY WAY DARK MATTER HALO FROM THE SAGITTARIUS STELLAR TIDAL STREAM
Law, D. R., Majewski, S. R., & Johnston, K. V. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/703/1/l67 · Cited by 163
A new determination of the local dark matter density from the kinematics of K dwarfs
Garbari, S., Liu, C., Read, J. I., & Lake, G. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21608.x · Cited by 155 · cited 2×
“The value we find (0.0100± 0.0010 M⊙ pc−3) is larger than many of the local measures in the compilation (though not all, e.g.,Garbari et al. 2012, when no strong prior on the baryonic component is invoked).”
BackgroundInfluentialThe Bar and Spiral Structure Legacy (BeSSeL) Survey: Mapping the Milky Way with VLBI Astrometry†
Brunthaler, A., Reid, M., Menten, K., Zheng, X., Bartkiewicz, A., Choi, Y., Dame, T., Hachisuka, K., Immer, K., Moellenbrock, G., et al. (2011) · Astronomische Nachrichten · doi:10.1002/asna.201111560 · Cited by 153 · cited 1×
“Reid et al. (2014) summarised the work of a number of groups, most notably the Bar and Spiral Structure Legacy survey (BeSSeL,Brunthaler et al. 2011) and VLBI Exploration of Radio Astronomy (VERA,Honma et al. 2000), which have determined the parallaxes, proper motions and line-of-sight velocities…”
BackgroundThe uncertainty in Galactic parametersPreprint
Mcmillan, P. J., & Binney, J. J. (2010) · Cited by 145
Self-citationBinney, J. J., & McMillan, P. J. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18268.x · Cited by 137 · cited 1×
“…(and used similar constraints from maser sources to those used in this study), andBovy & Rix (2013) who fit quasi-isothermal distribution functions (Binney & McMillan 2011) to ‘mono-abundance populations’ (groups of stars in a small range of [Fe/H] and [α/Fe]) from the SEGUE survey (Yanny et al.…”
MethodSelf-citationBroken degeneracies: the rotation curve and velocity anisotropy of the Milky Way halo
Deason, A. J., Belokurov, V., Evans, N. W., & An, J. (2012) · Monthly Notices of the Royal Astronomical Society: Letters · doi:10.1111/j.1745-3933.2012.01283.x · Cited by 133 · cited 1×
“Deason et al.(2012) and Xue et al. (2008) used samples of blue horizontal branch stars to determine the mass contained within 50 and 60 kpc (respectively).”
MethodWilson, J. C., Hearty, F., Skrutskie, M. F., Majewski, S. R., Schiavon, R. P., Eisenstein, D. J., Gunn, J., Blank, B., Henderson, C., Smee, S. A., et al. (2010) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.856708 · Cited by 131
KINEMATIC MODELING OF THE MILKY WAY USING THE RAVE AND GCS STELLAR SURVEYS
Sharma, S., Bland‐Hawthorn, J., Binney, J. J., Freeman, K. C., Steinmetz, M., Boeche, C., Bienaymé, O., Gibson, B. K., Gilmore, G. F., Grebel, E. K., et al. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/793/1/51 · Cited by 130 · cited 1×
“Sharma et al.(2014) noted that the use of Gaussian models of the kind used byBovy et al.(2012b) can lead to this behaviour in the model velocity dispersion where other models do not, because the Gaussian model is unable to properly represent the skewness of thevφ distribution.”
MethodThe Vertical Distribution and Kinematics of H i and Mass Models of the Galactic Disk
Malhotra, S. (1995) · The Astrophysical Journal · doi:10.1086/175946 · Cited by 128 · cited 1×
“As in Paper I we use the terminal velocity curve determined by Malhotra(1994, 1995) to constrain the rotation curve forR < R0.”
MethodGlobal properties of the Hi distribution in the outer Milky Way. Planar and extra-planar gasPreprint
Kalberla, P. M. W., & Dedes, L. (2007) · Cited by 124
Chemodynamics Of The Milky Way I. The First Year Of APOGEE Data
Anders, F., Chiappini, C., Santiago, B. X., Rocha–Pinto, H. J., Girardi, L., da Costa, L. N., Maia, M. A. G., Steinmetz, M., Minchev, I., Schultheis, M., et al. (2013) · Americanae (AECID Library) · doi:10.15781/t29j71 · Cited by 116
Seeing Through the Dust: The Detection of HI and the Exploration of the ISM in Galaxies
Taylor, A. R., Landecker, T. L., & Willis, A. G. (2002) · ASPC · Cited by 116
Holt, S. S., & Verter, F. (1993) · Cited by 113
The Vertical Distribution and Kinematics of HI and Mass Models of the Galactic DiskPreprint
Malhotra, S. (1994) · Cited by 113
Weighing the local dark matter with RAVE red clump stars
Bienaymé, O., Famaey, B., Siebert, A., Freeman, K. C., Gibson, B. K., Gilmore, G., Grebel, E. K., Bland-Hawthorn, J., Kordopatis, G., Munari, U., et al. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201424478 · Cited by 112 · cited 1×
“Piffl et al. (2014a) argued that combining their results with those of Bienaymé et al.(2014) provided tentative indications of an axis ratio (in the isodensity contours) ofq ∼ 0.8.”
ResultInfluentialLuminous and dark matter in the Milky Way
Olling, R. P., & Merrifield, M. R. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04581.x · Cited by 111
A review of action estimation methods for galactic dynamics
Sanders, J. L., & Binney, J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw106 · Cited by 111
The mechanics of tidal streams
Eyre, A., & Binney, J. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.18270.x · Cited by 105 · cited 1×
“Thedifference between the motion on these orbits is the primary influence on the observed structure of the stream (Eyre & Binney 2011).”
BackgroundGround-based and Airborne Instrumentation for Astronomy III
McLean, I. S., Ramsay, S. K., & Takami, H. (2010) · Cited by 103
Dipping our toes in the water: first models of GD-1 as a stream
Bowden, A., Belokurov, V. A., & Evans, N. W. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv285 · Cited by 94
Weighing the local dark matter with RAVE red clump stars
Bienaymé, O., Famaey, B., Siebert, A., Freeman, K. C., Gibson, B. K., Gilmore, G. F., Grebel, E. K., Bland‐Hawthorn, J., Kordopatis, G., Munari, U., et al. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201424478/pdf · Cited by 93
The vertical equilibrium of molecular gas in the Galactic disk
Malhotra, S. (1994) · The Astrophysical Journal · doi:10.1086/174677 · Cited by 92 · cited 1×
“As in Paper I we use the terminal velocity curve determined by Malhotra(1994, 1995) to constrain the rotation curve forR < R0.”
MethodBroken degeneracies: the rotation curve and velocity anisotropy of the Milky Way haloPreprint
Deason, A. J., Belokurov, V. A., Evans, N. W., & An, J. (2012) · Cited by 89
Luminous and Dark Matter in the Milky WayPreprint
Olling, R. P., & Merrifield, M. R. (2001) · Cited by 85
THE POWER SPECTRUM OF THE MILKY WAY: VELOCITY FLUCTUATIONS IN THE GALACTIC DISK
Bovy, J., Bird, J. C., Pérez, A. E. G., Majewski, S. R., Nidever, D. L., & Zasowski, G. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/800/2/83 · Cited by 82
The TMT instrumentation program
Simard, L., Crampton, D., Ellerbroek, B. L., & Boyer, C. (2010) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.857187 · Cited by 79
Ibata, R. A., Lewis, G. F., & Martin, N. F. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/819/1/1 · Cited by 74 · cited 1×
“However,Ibata et al.(2016) used deeper photometry of these tidal tails to demonstrate that these overdensities are very likely to be observational artefacts associated with inhomogeneities in the SDSS photometry used to produce the maps of Palomar 5 used byKüpper et al., (see alsoThomas et al.…”
MethodIncorrect rotation curve of the Milky Way
Chemin, L., Renaud, F., & Soubiran, C. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526040 · Cited by 67
THE SURFACE DENSITY PROFILE OF THE GALACTIC DISK FROM THE TERMINAL VELOCITY CURVE
McGaugh, S. (2015) · The Astrophysical Journal · doi:10.3847/0004-637x/816/1/42 · Cited by 62
2011. The mechanics of tidal streamsPreprint
Eyre, A., & Binney, J. (2016) · Cited by 61
Distance to NGC 281 in a Galactic Fragmenting Superbubble: Parallax Measurements with VERA
Sato, M., Hirota, T., Honma, M., Kobayashi, H., Sasao, T., Bushimata, T., Choi, Y. K., Imai, H., Iwadate, K., Jike, T., et al. (2008) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/60.5.975 · Cited by 59 · cited 1×
“We also allow for the possibility that a few of these objects may be strongly forced from a circular orbit by supernovae (e.g.Sato et al. 2008), by having a two-Gaussian pdf around this central value, with the broader Gaussian component being there to deal with these outliers.”
BackgroundSpiral Galaxies in the Near-IR
Minniti, D., & Rix, H. (1996) · ESO astrophysics symposia · doi:10.1007/978-3-540-49739-4 · Cited by 56
THE MILKY WAY TOMOGRAPHY WITH SLOAN DIGITAL SKY SURVEY. V. MAPPING THE DARK MATTER HALO
Loebman, S., Ivezić, Ž., Quinn, T. R., Bovy, J., Christensen, C., Jurić, M., Roškar, R., Brooks, A. M., & Governato, F. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/794/2/151 · Cited by 55 · cited 1×
“…halo as seen by the SDSS survey has yielded claims of constraints on the shape of the equipotential surfaces of the halo ranging from oblate with axis ratioqΦ = 0.7±0.1 (corresponding to axis ratios in the density distribution of 0.4± 0.1, Loebman et al. 2014) to prolate with axis ratio 1.5 . qΦ .”
BackgroundInfluentialIncorrect rotation curve of the Milky Way
Chemin, L., Renaud, F., & Soubiran, C. (2015) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201526040/pdf · Cited by 49
Analysing surveys of our Galaxy – II. Determining the potential
McMillan, P. J., & Binney, J. J. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt814 · Cited by 46 · cited 2×
“It also provides a helpful estimate of the potential that can be refined by dynamical modelling (e.g.McMillan & Binney 2013; Bovy & Rix 2013; Piffl et al. 2014a).”
BackgroundMethodSelf-citationTorus mapper: a code for dynamical models of galaxies
Binney, J. J., & McMillan, P. J. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2734 · Cited by 45 · cited 1×
“The stars seen byGaia orbit in the potential of the Milky Way, and it is the nature of their orbits (best characterised by their actions, e.g.Binney & McMillan 2016) that are generally of real interest for understanding Galactic structure, rather than their exact positions and velocities at this…”
BackgroundSelf-citationThe distribution of neutral gas in the Milky Way
Dame, T. M. (1992) · AIP conference proceedings · doi:10.1063/1.43985 · Cited by 42
Galactic rotation curve and spiral density wave parameters from 73 masers
Бобылев, В. В., & Bajkova, A. T. (2013) · Astronomy Letters · doi:10.1134/s1063773713120037 · Cited by 32 · cited 1×
“They have therefore been used by numerous authors to constrain the properties of the Milky Way (e.g.,Reid et al. 2009a; McMillan & Binney 2010; Bovy et al. 2009; Bobylev & Bajkova 2013; Reid et al. 2014, Paper I).”
MethodExploring the reality of density substructures in the Palomar 5 stellar stream
Thomas, G. F., Ibata, R., Famaey, B., Martin, N. F., & Lewis, G. F. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1189 · Cited by 32
Towards a Three-Dimensional Model of the Galaxy
Spergel, D. N., Malhotra, S., & Blitz, L. (1996) · ESO astrophysics symposia · doi:10.1007/978-3-540-49739-4_19 · Cited by 29
Rotational signature of the Milky Way stellar halo
Fermani, F., & Schönrich, R. A. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt597 · Cited by 28 · cited 2×
“Fermani & Schönrich(2013) raise important concerns regarding the selection of stars for these studies7.”
BackgroundJ-Net Galactic Plane Survey of VLBI Radio Sources for VLBI Exploration of Radio Astrometry (VERA)Preprint
Honma, M., Oyama, T., Hachisuka, K., Sawada‐Satoh, S., Sebata, K., Sekido, M., Suzuyama, T., Ichikawa, R., Kondo, T., Sakai, K., et al. (2016) · Cited by 22
J-Net Galactic-Plane Survey of VLBI Radio Sources for VLBI Exploration of Radio Astrometry (VERA)
Honma, M., Oyama, T., Hachisuka, K., Sawada-Satoh, S., Sebata, K., Miyoshi, M., Kameya, O., Manabe, S., Kawaguchi, N., Sasao, T., et al. (2000) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/52.4.631 · Cited by 20 · cited 1×
“…the work of a number of groups, most notably the Bar and Spiral Structure Legacy survey (BeSSeL,Brunthaler et al. 2011) and VLBI Exploration of Radio Astronomy (VERA,Honma et al. 2000), which have determined the parallaxes, proper motions and line-of-sight velocities of 103 Galactic HMSFRs.”
BackgroundThe difficulty of measuring the local dark matter density
Hessman, F. V. (2015) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201526022 · Cited by 19 · cited 1×
“This is not made clear in KD08, and this has led some authors to (mistakenly) add a∼40 per cent correction for helium and metals (e.g.Hessman 2015).”
BackgroundThe difficulty of measuring the local dark matter density
Hessman, F. V. (2015) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201526022/pdf · Cited by 19
HI and Galactic StructurePreprint
Lockman, F. J. (2002) · arXiv (Cornell University) · doi:10.48550/arxiv.astro-ph/0203210 · Cited by 1
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Cited by
Sorted by citations
Naiman, J., Pillepich, A., Springel, V., Ramirez-Ruiz, E., Torrey, P., Vogelsberger, M., Pakmor, R., Nelson, D., Marinacci, F., Hernquist, L., et al. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty618 · Cited by 693
“First, we select for galaxies with a total halo mass, M200,crit, in the range (0.6−2)×1012 M (Eadie et al. 2015; McMillan 2017; Zaritsky & Courtois 2017), which results in approximately 2000 galaxies.”
MethodInfluentialThe merger that led to the formation of the Milky Way’s inner stellar halo and thick disk
Helmi, A., Babusiaux, C., Koppelman, H. H., Massari, D., Veljanoski, J., & Brown, A. G. A. (2018) · Nature · doi:10.1038/s41586-018-0625-x · Cited by 1,235
Formation of Double Neutron Star Systems
Tauris, T. M., Kramer, M., Freire, P. C. C., Wex, N., Janka, H., Langer, N., Podsiadlowski, P., Bozzo, E., Chaty, S., Kruckow, M. U., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7e89 · Cited by 693
“Finally, to convert the SSB velocity vector to the LSR we have used the Galactic model of McMillan (2017).”
MethodHelmi, A., van Leeuwen, F., McMillan, P. J., Massari, D., Antoja, T., Robin, A. C., Lindegren, L., Bastian, U., Arenou, F., Babusiaux, C., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832698 · Cited by 648
“We have found relatively small differences in the orbits in three different realistic Galactic potentials when we integrated over short timescales (the potentials are based on Allen & San- Article number, page 22 of 49 tillan 1991; Robin et al. 2003; McMillan 2017).”
InfluentialSelf-citationThe GALAH+ survey: Third data release
Buder, S., Sharma, S., Kos, J., Amarsi, A. M., Nordlander, T., LIND, K., Martell, S. L., Asplund, M., Bland‐Hawthorn, J., Casey, A. R., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1242 · Cited by 680
“For our calculations we use the best fitting axisymmetric potential by McMillan (2017) with a Solar radius of 8.21 kpc, consistent with the latest measurement by Gravity Collaboration et al. (2019) of 8.178 ± 0.013stat.”
MethodInfluential
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
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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