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Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution
Open accessAbstract
We construct a large set of dynamical models of the galactic bulge, bar and inner disc using the made-to-measure method. Our models are constrained to match the red clump giant density from a combination of the VVV, UKIDSS and 2MASS infrared surveys together with stellar kinematics in the bulge from the BRAVA and OGLE surveys, and in the entire bar region from the ARGOS Survey. We are able to recover the bar pattern speed and the stellar and dark matter mass distributions in the bar region, thus recovering the entire galactic effective potential. We find a bar pattern speed of 39.0 ± 3.5 km s− 1 kpc− 1, placing the bar corotation radius at 6.1 ± 0.5 kpc and making the Milky Way bar a typical fast rotator. We evaluate the stellar mass of the long bar and bulge structure to be Mbar/bulge = 1.88 ± 0.12 × 1010 M⊙, larger than the mass of disc in the bar region, Minner disc = 1.29 ± 0.12 × 1010 M⊙. The total dynamical mass in the bulge volume is 1.85 ± 0.05 × 1010 M⊙. Thanks to more extended kinematic data sets and recent measurement of the bulge initial mass function, our models have a low dark matter fraction in the bulge of 17 ± 2 per cent. We find a dark matter density profile which flattens to a shallow cusp or core in the bulge region. Finally, we find dynamical evidence for an extra central mass of ∼ 0.2 × 1010 M⊙, probably in a nuclear disc or discy pseudo-bulge.
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Katz, D., Antoja, T., Romero-Gómez, M., Drimmel, R., Reylé, C., Seabroke, G. M., Soubiran, C., Babusiaux, C., Matteo, P. D., Figueras, F., et al. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832865 · Cited by 417
The Circular Velocity Curve of the Milky Way from 5 to 25 kpc
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Self-citationThe 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
“Also, for the same reason we do not model the complicated geometry of the stellar distribution at the centre of the MW, i.e. peanut bulge and bar (e.g. Portail et al. 2017), since it has only minor effects on the gravitational field at R > 5 kpc.”
BackgroundThe 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
“Also, for the same reason we do not model the complicated geometry of the stellar distribution at the centre of the MW, i.e. peanut bulge and bar (e.g. Portail et al. 2017), since it has only minor effects on the gravitational field at R > 5 kpc.”
BackgroundThe Circular Velocity Curve of the Milky Way from 5 to 25 kpc
Eilers, A., Hogg, D., Rix, H., & Ness, M. (2019) · MPG.PuRe (Max Planck Society) · Cited by 303
Self-citationPrimordial black holes as generators of cosmic structures
Carr, B. J., & Silk, J. I. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1204 · Cited by 332
Footprints of the Sagittarius dwarf galaxy in the Gaia data set
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Anders, F., Khalatyan, A., Queiroz, A. B. A., Chiappini, C., Ardèvol, J., Casamiquela, L., Figueras, F., Jiménez-Arranz, Ó., Jordi, C., Monguió, M., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142369 · Cited by 261
Bovy, J., Leung, H. W., Hunt, J. D., Mackereth, J. T., García-Hernández, D. A., & Roman–Lopes, A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2891 · Cited by 214
“…and uncertain data modeling, range from ≈ 30 km s−1 kpc−1 (RodriguezFernandez & Combes 2008) to ≈ 60 km s−1 kpc−1 (Englmaier & Gerhard 1999), with recent measurements (Portail et al. 2017; Sanders et al. 2019) clustering around 40 km s−1 kpc−1, in good agreement with our simple determination here.”
BackgroundChemodynamical History of the Galactic Bulge
Barbuy, B., Chiappini, C., & Gerhard, O. (2018) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081817-051826 · Cited by 224
Self-citationBar, N., Blas, D., Blum, K., & Sibiryakov, S. M. (2018) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.98.083027 · Cited by 191
“[53] found dynamical evidence for the presence of a mass component of ∼2 × 10(9) M⊙ extending to ∼250 pc.”
BackgroundMethodChemodynamical History of the Galactic Bulge
Barbuy, B., Chiappini, C., & Gerhard, O. (2018) · MPG.PuRe (Max Planck Society) · Cited by 189
Self-citationLeung, H. W., & Bovy, J. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2245 · Cited by 169
“But our chemical Milky Way maps provide the first direct evidence from abundance ratios that the bar region extends out to 5 kpc, consistent with a fast-rotating, long bar as found by Portail et al. (2017).”
Steinmetz, M., Guiglion, G., McMillan, P. J., Matijevič, G., Enke, H., Kordopatis, G., Zwitter, T., Valentini, M., Chiappini, C., Casagrande, L., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab9ab8 · Cited by 168
Self-citationGaia Data Release 2: Mapping the Milky Way disc kinematics
Romero-Gómez, M., Figueras, F., Jordi, C., Luri, X., Fabricius, C., Masana, E., Portell, J., Clotet, M., Roca, J. T., Garzón, A., et al. (2018) · Dipòsit Digital de la Universitat de Barcelona (Universitat de Barcelona) · Cited by 160
A dark matter profile to model diverse feedback-induced core sizes of ΛCDM haloes
Lazar, A., Bullock, J. S., Boylan-Kolchin, M., Chan, T. K., Hopkins, P. F., Graus, A. S., Wetzel, A. R., El-Badry, K., Wheeler, C., Straight, M. C., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2101 · Cited by 193
“Portail et al. (2017) find evidence for a dark matter core comparable in size to what we quantify our feedback-affected MW-mass haloes.”
BackgroundGaia Data Release 2. Mapping the Milky Way disc kinematics
Katz, D., Antoja, T., Romero-Gómez, M., Drimmel, R., Reylé, C., Seabroke, G. M., Soubiran, C., Babusiaux, C., Matteo, P. D., Figueras, F., et al. (2018) · UCrea (University of Cantabria) · doi:10.48350/158407 · Cited by 154
The pattern speed of the Milky Way bar from transverse velocities
Sanders, J. L., Smith, L. C., & Evans, N. W. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1827 · Cited by 152
“This simulation is designed to approximately match the properties of the Milky Way although not to the level of detail of a full Made-to-Measure model (Portail et al. 2017).”
MethodResultInfluentialDrimmel, R., Romero-Gómez, M., Chemin, L., Ramos, P., Poggio, E., Ripepi, V., Andrae, R., Blomme, R., Cantat-Gaudin, T., Castro-Ginard, A., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243797 · Cited by 172
The dark matter profile of the Milky Way inferred from its circular velocity curve
Ou, X., Eilers, A., Necib, L., & Frebel, A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae034 · Cited by 161
Revisiting the Tale of Hercules: How Stars Orbiting the Lagrange Points Visit the Sun
Pérez-Villegas, Á., Portail, M., Wegg, C., & Gerhard, O. (2017) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aa6c26 · Cited by 125
“We have analyzed the velocity distribution in the SNd using the best M2M particle model of the Galaxy of Portail et al. (2017) fitted to a variety of inner Galaxy data.”
BackgroundMethodResultInfluentialSelf-citationThe Fermi-LAT GeV excess as a tracer of stellar mass in the Galactic bulge
Bartels, R., Storm, E., Weniger, C., & Calore, F. (2018) · Nature Astronomy · doi:10.1038/s41550-018-0531-z · Cited by 122
Novel constraints on the particle nature of dark matter from stellar streams
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Deep Search for Decaying Dark Matter with XMM-Newton Blank-Sky Observations
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The Milky Way bar and bulge revealed by APOGEE and Gaia EDR3
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A Testable Conspiracy: Simulating Baryonic Effects on Self-interacting Dark Matter Halos
Elbert, O. D., Bullock, J. S., Kaplinghat, M., Garrison-Kimmel, S., Graus, A. S., & Rocha, M. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aa9710 · Cited by 114
Rotation Curves in z ∼ 1–2 Star-forming Disks: Evidence for Cored Dark Matter Distributions
Genzel, R., Price, S. H., Übler, H., Schreiber, N. M. F., Shimizu, T., Tacconi, L. J., Bender, R., Burkert, A. M., Contursi, A., Coogan, R. T., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abb0ea · Cited by 119
Klioner, S. A., Mignard, F., Lindegren, L., Bastian, U., McMillan, P. J., Hernández, J., Hobbs, D., Ramos-Lerate, M., Biermann, M., Bombrun, A., et al. (2021) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202039734 · Cited by 120
Resonance sweeping by a decelerating Galactic bar
Chiba, R., Friske, J. K. S., & Schönrich, R. A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3585 · Cited by 103
“…al. (2019) both derived p = 41 ± 3 km s−1 kpc−1 by applying the continuity equation to stars in the bulge; With madeto-measure models in the bar region, Portail et al. (2017) deduced p = 39 ± 3.5 km s−1 kpc−1 and Clarke et al. (2019) estimated, from fitting to proper motion data, p = 37.5 km s−1…”
MethodResultInfluentialThe gravitational force field of the Galaxy measured from the kinematics of RR Lyrae in Gaia
Wegg, C., Gerhard, O., & Bieth, M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz572 · Cited by 104
“These mock halos were constructed from the made-to-measure models of the inner Galaxy constructed by Portail et al. (2017).”
BackgroundMethodSelf-citationParsa, M., Eckart, A., Shahzamanian, B., Karas, V., Zajaček, M., Zensus, J. A., & Straubmeier, C. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa7bf0 · Cited by 102
“The quantity R0 is an essential basis for understanding and modeling the Galactic dynamics (e.g., Englmaier & Gerhard 1999; Portail et al. 2017).”
BackgroundSignatures of the resonances of a large Galactic bar in local velocity space
Monari, G., Famaey, B., Siebert, A., Wegg, C., & Gerhard, O. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201834820 · Cited by 103
Self-citationFluctuations in galactic bar parameters due to bar–spiral interaction
Hilmi, T., Minchev, I., Buck, T., Martig, M., Quillen, A. C., Monari, G., Famaey, B., de Jong, R. S., Laporte, C. F. P., Read, J. I., et al. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1934 · Cited by 100
“Starting with Wegg et al. (2015), Sormani et al. (2015), Li et al. (2016), and Portail et al. (2017), more recent works using different datasets and methods have suggested a significantly longer bar than previously thought (∼ 5 kpc) and a pattern speed much lower than previously accepted (35−45 km…”
BackgroundMethodResultInfluentialSelf-citationSimulations of the Milky Way’s Central Molecular Zone – II. Star formation
Sormani, M. C., Treß, R. G., Glover, S. C. O., Klessen, R. S., Battersby, C., Clark, P. C., Hatchfield, H. P., & Smith, R. J. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1999 · Cited by 105
Sormani, M. C., & Barnes, A. T. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz046 · Cited by 97
“The bar is assumed to rotate rigidly with a constant pattern speed of Ωp = 40kms−1 kpc−1, as implied by recent estimates (Sormani et al. 2015b; Portail et al. 2017; Pérez-Villegas et al. 2017).”
MethodDynamical constraints on a dark matter spike at the Galactic centre from stellar orbits
Lacroix, T. (2018) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201832652 · Cited by 89
The Milky Way bar/bulge in proper motions: a 3D view from VIRAC and Gaia
Clarke, J. P., Wegg, C., Gerhard, O., Smith, L. C., Lucas, P. W., & Wylie, S. M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2382 · Cited by 90
“…LF representing the bulge stellar population, we used (i) the Kroupa initial mass function (Kroupa 2001) as measured in the bulge (Wegg, Gerhard & Portail 2017); (ii) a kernel-smoothed metallicity distribution in Baade’s window from Zoccali et al. (2008) where we use the metallicity measurement…”
MethodSelf-citationSelf-consistent modelling of the Milky Way’s nuclear stellar disc
Sormani, M. C., Sanders, J. L., Fritz, T. K., Smith, L. C., Gerhard, O., Schödel, R., Magorrian, J., Neumayer, N., Nogueras-Lara, F., Feldmeier-Krause, A., et al. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac639 · Cited by 77
Self-citationEffects of Gas on Formation and Evolution of Stellar Bars and Nuclear Rings in Disk Galaxies
Seo, W.-Y., Kim, W., Kwak, S., Hsieh, P.-Y., Han, C., & Hopkins, P. F. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aafc5f · Cited by 98
Tree-ring structure of Galactic bar resonance
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Fragkoudi, F., Katz, D., Trick, W. H., White, S. D. M., Matteo, P. D., Sormani, M. C., Александрович, Х. С., Haywood, M., Hallé, A., & Gómez, A. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1875 · Cited by 81
“In this scenario, the thin bar of the Milky Way may extend up to 5 kpc (Wegg & Gerhard 2013; Portail et al. 2017), which would make it longer than the corotation radius of ∼4 kpc in the classical short/fast bar scenario.”
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Banik, N., Bovy, J., Bertone, G., Erkal, D., & de Boer, T. J. L. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab210 · Cited by 80
Stellar streams in the Gaia era
Bonaca, A., & Price-Whelan, A. M. (2024) · New Astronomy Reviews · doi:10.1016/j.newar.2024.101713 · Cited by 87
Recognizing Axionic Dark Matter by Compton and de Broglie Scale Modulation of Pulsar Timing
Martino, I. D., Broadhurst, T. J., Tye, S.-H. H., Chiueh, T., Schive, H.-Y., & Lazkoz, R. (2017) · Physical Review Letters · doi:10.1103/physrevlett.119.221103 · Cited by 80
Tracing the Hercules stream with Gaia and LAMOST: new evidence for a fast bar in the Milky Way
Monari, G., Kawata, D., Hunt, J. A. S., & Famaey, B. (2016) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slw238 · Cited by 79
Effects of baryonic and dark matter substructure on the Pal 5 stream
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Strong constraints on thermal relic dark matter from Fermi-LAT observations of the Galactic Center
Abazajian, K. N., Horiuchi, S., Kaplinghat, M., Keeley, R. E., & Macías, O. (2020) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.102.043012 · Cited by 88
Ultralight dark matter in disk galaxies
Bar, N., Blum, K., Eby, J., & Sato, R. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.99.103020 · Cited by 76
“A kinematic detection supporting the disk-like morphology of the NSD was given in [55], and the mass and approximate scale estimates are consistent with the dynamical modelling of [56] and with microlensing analyses [57] that probe the outer boundary of the NSD region.”
ResultIbata, R., Malhan, K., Tenachi, W., Arentsen, A., Bellazzini, M., Bianchini, P., Bonifacio, P., Caffau, E., Diakogiannis, F. I., Errani, R., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad382d · Cited by 108
Haywood, M., di Matteo, P., Lehnert, M., Snaith, O., Fragkoudi, F., & Khoperskov, S. (2018) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201731363 · Cited by 43
“In the MW, the exact position of the OLR is debated: slightly inside the solar orbit (Dehnen 2000), or further away (e.g., Pérez-Villegas et al. 2017, who, after the work of Portail et al. 2017, proposed that it is situated at 10.5 kpc).”
BackgroundInfluentialA measurement of the distance to the Galactic centre using the kinematics of bar stars
Leung, H. W., Bovy, J., Mackereth, J. T., Hunt, J. D., Lane, R. R., & Wilson, J. C. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3529 · Cited by 80
Identifying resonances of the Galactic bar in Gaia DR2: I. Clues from action space
Trick, W. H., Fragkoudi, F., Hunt, J. D., Mackereth, J. T., & White, S. D. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3317 · Cited by 69
REBELS-25: discovery of a dynamically cold disc galaxy at z = 7.31
Rowland, L. E., Hodge, J., Bouwens, R. J., Piña, P. E. M., Hygate, A. P. S., Algera, H., Aravena, M., Bowler, R. A. A., da Cunha, E., Dayal, P., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae2217 · Cited by 71
Chemodynamical modelling of the galactic bulge and bar
Portail, M., Wegg, C., Gerhard, O., & Ness, M. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1293 · Cited by 70
“We applied the method based on the dynamical model of the bar region recently made by Portail et al. (2017), and successfully reproduced the spatial and kinematic variations of the metallicities of stars seen in the ARGOS and APOGEE (DR12) surveys.”
MethodSelf-citationThree mechanisms for bar thickening
Sellwood, J. A., & Gerhard, O. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1336 · Cited by 71
“Although our models were not intended to match the Milky Way, in which the inner halo has a lower density (Portail et al. 2017), we nevertheless scale them to the Milky Way.”
BackgroundMethodSelf-citationBroken into Pieces: ATLAS and Aliqa Uma as One Single Stream
Li, T. S., Koposov, S. E., Erkal, D., Ji, A., Shipp, N., Pace, A., Hilmi, T., Kuehn, K., Lewis, G., Mackey, D., et al. (2020) · Astrophysical Journal · doi:10.3847/1538-4357/abeb18 · Cited by 57
Александрович, Х. С., Gerhard, O., Matteo, P. D., Haywood, M., Katz, D., Khrapov, S. S., Khoperskov, A. V., & Arnaboldi, M. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936645 · Cited by 68
“For the significantly declining rotation curve of the Milky Way (Eilers et al. 2019) we obtain L8, page 4 of 9 values of 37−42 km s−1 kpc−1 in good agreement with recent in situ estimates from Milky Way bar kinematics and dynamics (Portail et al. 2017; Sanders et al. 2019; Bovy et al. 2019).”
MethodSelf-citationMilky Way dynamics in light of Gaia
Hunt, J. D., & Vasiliev, E. (2025) · New Astronomy Reviews · doi:10.1016/j.newar.2024.101721 · Cited by 87
Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere
Chavanis, P.-H. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.100.083022 · Cited by 78
Gas Dynamics in the Galaxy: Total Mass Distribution and the Bar Pattern Speed
Li, Z., Shen, J., Gerhard, O., & Clarke, J. P. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac3823 · Cited by 66
Self-citationPopSyCLE: A New Population Synthesis Code for Compact Object Microlensing Events
Lam, C. Y., Lu, J. R., Hosek, M. W., Dawson, W. A., & Golovich, N. R. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab5fd3 · Cited by 64
Anatomy of Eddington-like inversion methods in the context of dark matter searches
Lacroix, T., Stref, M., & Lavalle, J. (2018) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2018/09/040 · Cited by 63
The Bulge Radial Velocity Assay for RR Lyrae Stars (BRAVA-RR) DR2: A Bimodal Bulge?
Kunder, A., Pérez-Villegas, Á., Rich, R. M., Ogata, J., Murari, E., Boren, E., Johnson, C. I., Nataf, D., Walker, A., Bono, G., et al. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/ab8d35 · Cited by 64
The bar and spiral arms in the Milky Way: structure and kinematics
Shen, J., & Zheng, X.-W. (2020) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/20/10/159 · Cited by 62
Distribution and kinematics of atomic and molecular gas inside the solar circle
Marasco, A., Fraternali, F., van der Hulst, J. M., & Oosterloo, T. (2017) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201731054 · Cited by 61
“…more gently than what can be derived from a simple tangent-point analysis of the l − v diagrams: this was first recognised by Binney et al. (1991), and considered recently by dynamical models of the inner Galactic disc based on the density and kinematics of stars (Portail et al. 2017; see also Fig.”
BackgroundInfluentialThe stellar mass distribution of the Milky Way’s bar: an analytical model
Sormani, M. C., Gerhard, O., Portail, M., Vasiliev, E., & Clarke, J. P. (2022) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slac046 · Cited by 59
Self-citationSormani, M. C., Treß, R. G., Glover, S. C. O., Klessen, R. S., Barnes, A. T., Battersby, C., Clark, P. C., Hatchfield, H. P., & Smith, R. J. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2054 · Cited by 62
“…of the heating & cooling of the ISM and the pattern speed of the gas is independently constrained to be Ωp = 40kms−1 kpc−1 (e.g. Sormani et al. 2015b; Portail et al. 2017; Sanders et al. 2019), we have increased the strength of the bar (compatibly with with known observational constraints) to…”
BackgroundStars Behind Bars. I. The Milky Way's Central Stellar Populations
Buck, T., Ness, M., Macciò, A. V., Obreja, A., & Dutton, A. A. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac890 · Cited by 56
Self-citationBayesian reconstruction of the Milky Way dark matter distribution
Karukes, E., Benito, M. T. R., Fabio Iocco, A., Trotta, R., & Geringer-Sameth, A. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/09/046 · Cited by 56
Age dating the Galactic bar with the nuclear stellar disc
Baba, J., & Kawata, D. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa140 · Cited by 60
“Using kinematic data of the bar/bulge stars, recent studies suggest that the current pattern speed of the Galactic bar is about 40 km s−1 kpc−1 (Portail et al. 2017; Sanders, Smith & Evans 2019; Bovy et al. 2019), as opposed to a fast pattern speed inferred from the kinematics of the solar…”
BackgroundA new class of fossil fragments from the hierarchical assembly of the Galactic bulge
Ferraro, F. R., Pallanca, C., Lanzoni, B., Crociati, C., Dalessandro, E., Origlia, L., Rich, R. M., Saracino, S., Mucciarelli, A., Valenti, E., et al. (2020) · Nature Astronomy · doi:10.1038/s41550-020-01267-y · Cited by 55
Escapees from the bar resonances
Александрович, Х. С., Matteo, P. D., Haywood, M., Gómez, A., & Snaith, O. N. (2020) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201937188 · Cited by 53
“…et al. 2010; Fragkoudi et al. 2019), while some others claim that the bar OLR is outside the solar radius, and that – as a consequence – the Sun should lie between the bar CR and OLR (Wegg & Gerhard 2013; Portail et al. 2017; Sanders et al. 2019; Clarke et al. 2019; Khoperskov et al. 2019b).”
BackgroundSanders, J. L., Kawata, D., Matsunaga, N., Sormani, M. C., Smith, L. C., Minniti, D., & Gerhard, O. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae711 · Cited by 52
Self-citationExploring the Stellar Age Distribution of the Milky Way Bulge Using APOGEE
Hasselquist, S., Zasowski, G., Feuillet, D. K., Schultheis, M., Nataf, D. M., Anguiano, B., Beaton, R. L., Beers, T. C., Cohen, R. E., Cunha, K., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abaeee · Cited by 52
Stellar halo substructure generated by bar resonances
Dillamore, A. M., Belokurov, V. A., Evans, N. W., & Davies, E. Y. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2136 · Cited by 60
Novel constraints on fermionic dark matter from galactic observables I: The Milky Way
Argüelles, C. R., Krut, A., Rueda, J. A., & RUFFINI, R. J. (2018) · Physics of the Dark Universe · doi:10.1016/j.dark.2018.07.002 · Cited by 51
Dynamical evidence of a dark solitonic core of 109M⊙ in the milky way
Martino, I. D., Broadhurst, T. J., Tye, S.-H. H., Chiueh, T., & Schive, H.-Y. (2020) · Physics of the Dark Universe · doi:10.1016/j.dark.2020.100503 · Cited by 51
“Recently, Portail et al (2017) [27] have investigated a combination of data from VVV, UKIDSS and 2MASS infrared surveys together with kinematics data from the BRAVA and OGLE surveys to reconstruct the velocity field in the Milky Way’s bulge in the whole bulge area |l| 10◦ and −10◦ b +5◦.”
BackgroundResultInfluentialExploring the Galactic Warp through Asymmetries in the Kinematics of the Galactic Disk
Cheng, X., Anguiano, B., Majewski, S. R., Hayes, C. R., Arras, P., Chiappini, C., Hasselquist, S., Queiroz, A. B. A., Nıtschelm, C., García-Hernández, D. A., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/abc3c2 · Cited by 51
Transverse kinematics of the Galactic bar-bulge from VVV and Gaia
Sanders, J. L., Smith, L. C., Evans, N. W., & Lucas, P. W. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1630 · Cited by 49
“This agrees with the models of Portail et al. (2017), who found the Rattenbury et al. (2007) dispersions overpredict their model (their figure 16).”
BackgroundMethodResultInfluentialVariations in the Width, Density, and Direction of the Palomar 5 Tidal Tails
Bonaca, A., Pearson, S., Price-Whelan, A., Dey, A., Geha, M., Kallivayalil, N., Moustakas, J., Muñoz, R., Myers, A., Schlegel, D., et al. (2019) · Astrophysical Journal · doi:10.3847/1538-4357/ab5afe · Cited by 44
Revisiting MOA 2013-BLG-220L: A Solar-type Star with a Cold Super-Jupiter Companion
Vandorou, A., Bennett, D. P., Beaulieu, J., Alard, C., Blackman, J. W., Cole, A. A., Bhattacharya, A., Bond, I. A., Koshimoto, N., & Marquette, J. B. (2020) · The Astronomical Journal · doi:10.3847/1538-3881/aba2d3 · Cited by 48
Blaña, M., Gerhard, O., Wegg, C., Portail, M., Opitsch, M., Saglia, R. P., Fabricius, M., Erwin, P., & Bender, R. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2311 · Cited by 48
“The parameters of these target analytical profiles are determined during each M2M run similarly to Portail et al. (2017a), by fitting the dark matter halo profile together with the current stellar mass distribution to match: i) the dark matter mass enclosed within an ellipsoidal volume of the major…”
BackgroundMethodInfluentialSelf-citationDynamically constraining the length of the Milky way bar
Lucey, M., Pearson, S., Hunt, J. D., Hawkins, K., Ness, M., Petersen, M. S., Price-Whelan, A. M., & Weinberg, M. D. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad406 · Cited by 46
Self-citationNitschai, M. S., Cappellari, M., & Neumayer, N. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1128 · Cited by 47
“Portail et al. (2017) used the made-to-measure method to construct dynamical models of the bar region only, using kinematics from BRAVA, ARGOS, and OGLE and recovering the 1Relativistic corrections are unimportant here. bar pattern speed, and the stellar and dark matter mass distribution in this…”
MethodResultGlobular clusters in the inner Galaxy classified from dynamical orbital criteria
Pérez-Villegas, Á., Barbuy, B., Kerber, L. O., Ortolani, S., Souza, S. O., & Bica, E. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3162 · Cited by 55
Global torques and stochasticity as the drivers of massive black hole pairing in the young Universe
Bortolas, E., Capelo, P. R., Zana, T., Mayer, L., Bonetti, M., Dotti, M., Davies, M. B., & Madau, P. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2628 · Cited by 45
“Such structures are abundant in the local Universe (Kelvin et al. 2018 – a prominent example is our own Milky Way, Portail et al. 2017) and presumably at all times.”
BackgroundAbundances of disk and bulge giants from high-resolution optical spectra
Forsberg, R., Jönsson, H., Ryde, N., & Matteucci, F. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201936343 · Cited by 45
“However, with new findings and an accumulation of data, what we call the bulge is today predominately considered to be mainly the inner structures of the Galactic bar seen edge-on (e.g. Portail et al. 2017).”
BackgroundDistribution and kinematics of atomic and molecular gas inside the solar circle
Marasco, A., Fraternali, F., van der Hulst, J. M., & Oosterloo, T. A. (2017) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201731054/pdf · Cited by 45
Александрович, Х. С., & Gerhard, O. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202141836 · Cited by 49
Self-citationArentsen, A., Monari, G., Queiroz, A. B. A., Starkenburg, E., Martin, N. F., Chiappini, C., Aguado, D. S., Belokurov, V. A., Carlberg, R. G., Monty, S., et al. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae1049 · Cited by 52
Novel constraints on fermionic dark matter from galactic observables I: The Milky Way
Argüelles, C. R., Krut, A., Rueda, J. A., & RUFFINI, R. J. (2018) · El Servicio de Difusión de la Creación Intelectual (National University of La Plata) · Cited by 44
Testing kinematic distances under a realistic Galactic potential
Hunter, G. H., Sormani, M. C., Beckmann, J. P., Vasiliev, E., Glover, S. C. O., Klessen, R. S., Soler, J. D., Brucy, N., Girichidis, P., Göller, J., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202450000 · Cited by 52
Self-citationOn the orbits that generate the X-shape in the Milky Way bulge
Abbott, C. G., Valluri, M., Shen, J., & Debattista, V. P. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1262 · Cited by 43
“The most recent estimate (Portail et al. 2017) of the pattern frequency of the Milky Way bar is Ωp = 39.0 ± 3.5km s−1 kpc−1 (for a bar length 5.3 ± 0.36kpc).”
BackgroundInfluentialMultiple ultralight axionic wave dark matter and astronomical structures
Luu, H. N., Tye, S.-H. H., & Broadhurst, T. J. (2020) · Physics of the Dark Universe · doi:10.1016/j.dark.2020.100636 · Cited by 43
The COMBS Survey - II. Distinguishing the metal-poor bulge from the halo interlopers
Lucey, M., Hawkins, K., Ness, M., Debattista, V. P., Luna, A., Asplund, M., Bensby, T., Casagrande, L., Feltzing, S., Freeman, K. C., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab003 · Cited by 44
“In other words, it is possible that 3.5 kpc is too stringent of a cut and that many stars which participate in the bulge/bar may have apocenters > 3.5 kpc (Portail et al. 2017).”
BackgroundInfluentialSelf-citationDynamically Driven Inflow onto the Galactic Center and its Effect upon Molecular Clouds
Hatchfield, H. P., Sormani, M. C., Treß, R. G., Battersby, C., Smith, R. J., Glover, S. C. O., & Klessen, R. S. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac1e89 · Cited by 48
Eckner, C., Hou, X., Serpico, P. D., Winter, M., Zaharijaš, G., Martin, P., Mauro, M. D., Mirabal, N., Petrovic, J., Prodanovic, T., et al. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aac029 · Cited by 41
Wang, H., López-Corredoira, M., Huang, Y., Carlin, J. L., Chen, B., Wang, C., Chang, J., Zhang, H.-W., Xiang, M.-S., Yuan, H.-B., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3113 · Cited by 41
Hunting for heavy winos in the Galactic Center
Rinchiuso, L., Rodd, N. L., Moult, I., Moulin, E., Baumgart, M., Timothy Cohen, A., Slatyer, T. R., Stewart, I. W., & Vaidya, V. (2018) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.98.123014 · Cited by 40
“On the observational front, this means that going from gravitational measurements of the total mass density to limits on the DM density requires careful modeling of the baryonic component and has associated large systematic uncertainties, see, for instance, [35, 36].”
BackgroundMethod
Metadata
- Authors
- Portail, M., Gerhard, O., Wegg, C., & Ness, M.
- Affiliations
- Max Planck Institute for Extraterrestrial Physics (DE)
- Max Planck Institute for Astronomy (DE)
- Corresponding author
- Portail, Matthieu
- Gerhard, Ortwin
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2016-11-03
- Volume
- 465
- Issue
- 2
- Pages
- 1621-1644
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2555440354
- Cited by
- 378
- References
- 154
- Citations by year
- 2026: 37 · 2025: 44 · 2024: 46 · 2023: 23 · 2022: 30 · 2021: 42 · 2020: 51 · 2019: 42 · 2018: 35 · 2017: 26 · 2016: 2
- FWCI
- 16.71
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Max Planck Institute for Plasma Physics (submittedVersion)
- HighWire Press Open Archive (submittedVersion)
- MPG.PuRe (Max Planck Society) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- Galactic bulge, galactic bars, bar pattern speed, red clump giants, stellar kinematics, effective potential, nuclear discs
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