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Galaxy-induced transformation of dark matter haloes: Transformations of CDM haloes
Open accessAbstract
We use N-body/gasdynamical cosmological simulations to examine the effect of the assembly of a central galaxy on the shape and mass profile of its surrounding dark matter halo. Two series of simulations are compared; one that follows only the evolution of the dark matter component of individual haloes in the proper Λcold dark matter (ΛCDM) cosmological context, and a second series where a baryonic component is added and followed hydrodynamically. The simulations with baryons include radiative cooling but neglect the formation of stars and their feedback. The efficient, unimpeded cooling that results leads most baryons to collect at the halo centre in a centrifugally supported disc which, due to angular momentum losses, is too small and too massive when compared with typical spiral galaxies. This admittedly unrealistic model allows us, nevertheless, to gauge the maximum effect that galaxies may have in transforming their surrounding dark haloes. We find, in agreement with earlier work, that the shape of the halo becomes more axisymmetric: post galaxy assembly, haloes are transformed from triaxial into essentially oblate systems, with well-aligned isopotential contours of roughly constant flattening (〈c/a〉∼ 0.85). Haloes always contract as a result of galaxy assembly, but the effect is substantially less pronounced than predicted by the traditional ‘adiabatic-contraction’ hypothesis. The reduced contraction helps to reconcile ΛCDM haloes with constraints on the dark matter content inside the solar circle and should alleviate the longstanding difficulty of matching simultaneously the scaling properties of galaxy discs and the galaxy luminosity function. The halo contraction we report is also less pronounced than found in earlier simulations, a disagreement which suggests that halo contraction is not solely a function of the initial and final distribution of baryons. Not only how much baryonic mass has been deposited at the centre of a halo matters, but also the mode of its deposition. Although simple formulae might work in particular cases where galaxies form nearly adiabatically, in general it might prove impossible to predict the halo response to galaxy formation without a detailed understanding of a galaxy's detailed assembly history.
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“Nonetheless, individual haloes can deviate from the mean prediction since the size of the contraction is weakly dependent on the assembly history of the system (e.g. Abadi et al. 2010; Artale et al. 2019).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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In the citing paper
“This simplification is unlikely to affect our results since the baryonic distribution leads to a roughly spherical DM distribution in the inner regions, i.e. for r ≲ 20 kpc , which is the region where the best quality rotation curve data exists”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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In the citing paper
“Other simpler adiabatic contraction approximations, such as those used by Blumenthal et al. (1986) and Gnedin et al. (2004), tend systematically to under- or overpredict the halo contraction (e.g. Abadi et al. 2010; Duffy et al. 2010; Pedrosa et al. 2010; Dutton et al. 2016; Artale et al. 2019).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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Citations
Cites
Spergel, D. N., Verde, L., Peiris, H. V., Komatsu, E., Nolta, M. R., Bennett, C. L., Halpern, M., Hinshaw, G., Jarosik, N., Kogut, A., et al. (2003) · The Astrophysical Journal Supplement Series · doi:10.1086/377226 · Cited by 10,976 · cited 1×
“We adopt cosmological parameters consistent with the combined analysis of the 2dfGRS (Colless et al., 2001) and the first-year WMAP data (Spergel et al., 2003): a present day value of the Hubble constant of H0 = 70 km/s/Mpc; a scalefree initial density perturbation spectrum with no tilt and…”
MethodA Universal Density Profile from Hierarchical Clustering
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1997) · The Astrophysical Journal · doi:10.1086/304888 · Cited by 9,917 · cited 4×
“The DMO mass profile is shown by the thick red solid curve and, as expected, it is well approximated by the NFW (Navarro et al., 1996b, 1997) formula (thin solid line).”
BackgroundMethodInfluentialSelf-citationThe 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 · cited 4×
“The DMO mass profile is shown by the thick red solid curve and, as expected, it is well approximated by the NFW (Navarro et al., 1996b, 1997) formula (thin solid line).”
BackgroundMethodInfluentialSelf-citationA Universal Density Profile from Hierarchical ClusteringPreprint
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · Cited by 6,275
Self-citationSimulations 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×
“Each dot in this panel correspond to an NFW halo with concentration drawn at random from the mass-concentration relation (including scatter) derived by Neto et al. (2007) from the Millennium Simulation (Springel et al., 2005).”
MethodSelf-citationCroton, D. J., Springel, V., White, S. D. M., Lucia, G. D., Frenk, C. S., Gao, L., Jenkins, A., Kauffmann, G., Navarro, J. F., & Yoshida, N. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09675.x · Cited by 3,686 · cited 2×
“…formation have adopted this formulation in order to link the (observed) dynamical properties of luminous galaxies to the (predicted) properties of the dark halos that surround them (see, e.g., Mo et al., 1998; Cole et al., 2000; Dutton et al., 2005; Croton et al., 2006; Somerville et al., 2008).”
BackgroundSelf-citationStatistical Properties of X‐Ray Clusters: Analytic and Numerical Comparisons
Bryan, G. L., & Norman, M. L. (1998) · The Astrophysical Journal · doi:10.1086/305262 · Cited by 2,372 · cited 1×
“The virial density contrast, ∆vir(z) is given by ∆vir(z) = 18π 2 + 82f(z) − 39f(z)2, where f(z) = [Ω0(1 + z)3/(Ω0(1 + z)3 + ΩΛ))] − 1 and Ω0 = ΩCDM + Ωb(Bryan & Norman, 1998).”
The 2dF Galaxy Redshift Survey: spectra and redshifts
Colless, M., Dalton, G., Maddox, S., Sutherland, W. J., Norberg, P., Cole, S., Bland‐Hawthorn, J., Bridges, T. J., Cannon, R., Collins, C. A., et al. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04902.x · Cited by 2,368 · cited 1×
“We adopt cosmological parameters consistent with the combined analysis of the 2dfGRS (Colless et al., 2001) and the first-year WMAP data (Spergel et al., 2003): a present day value of the Hubble constant of H0 = 70 km/s/Mpc; a scalefree initial density perturbation spectrum with no tilt and…”
MethodThe formation of galactic discs
Mo, H. J., Mao, S., & White, S. D. M. (1998) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1998.01227.x · Cited by 2,166 · cited 2×
“…formation have adopted this formulation in order to link the (observed) dynamical properties of luminous galaxies to the (predicted) properties of the dark halos that surround them (see, e.g., Mo et al., 1998; Cole et al., 2000; Dutton et al., 2005; Croton et al., 2006; Somerville et al., 2008).”
BackgroundCole, S., Lacey, C. G., Baugh, C. M., & Frenk, C. S. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2000.03879.x · Cited by 1,952
Research works printed but not linked: 1
- Ma, 2004, Phys. Rev. Lett., 93, 1301
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Sorted by citations
Items 201–238 of 238
Narrow-band X-ray photometry as a tool for studying galaxy and cluster mass distributions
Humphrey, P. J., & Buote, D. A. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt1414 · Cited by 7
“…unique insight into the uncertain baryonic physics of galaxy formation, such as the role of feedback in shaping the nascent structures, and the complex interplay between adiabatic contraction and dynamical friction (e.g. Silk & Rees 1998; Gnedin et al. 2004; Hopkins et al. 2006; Abadi et al. 2010).”
BackgroundFirst measurement of the triaxiality of the inner dark matter halo of the Milky Way
Woudenberg, H. C., & Helmi, A. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451743 · Cited by 13
Accurate connected modeling of gas thermodynamics and matter distribution
Pandey, S., Salcido, J., To, C., Hill, J. C., Anbajagane, D., Baxter, E. J., & McCarthy, I. G. (2025) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.111.043529 · Cited by 6
Sensitivity of halo shape measurements
Fischer, M. S., & Valenzuela, L. M. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245031 · Cited by 6
Núñez-Castiñeyra, A., Nezri, E., Mollitor, P., Devriendt, J., & Teyssier, R. (2023) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2023/05/012 · Cited by 6
“The shape of DM halos in numerical simulations have been extensively studied with several techniques, using the mass distribution of the DM [51–65], or the gravitational potential induced by all the components of the simulations [66, 67], the latter having the advantage of reducing the fluctuations caused by the prese…”
MethodThe VIRUS-dE Survey. II. Cuspy and Round Halos in Dwarf Ellipticals—A Result of Early Assembly?
Lipka, M., Thomas, J., Saglia, R. P., Bender, R., Fabricius, M., & Partmann, C. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad7baa · Cited by 8
Dark matter in massive galaxies
Gerhard, O. (2012) · Proceedings of the International Astronomical Union · doi:10.1017/s174392131300481x · Cited by 6
“• The halo becomes more spherical and evolves towards oblate at all radii but mostly in its inner parts (Kazantzidis et al. 2004; Bailin et al. 2005; Berentzen & Shlosman 2006; Abadi et al. 2010).”
BackgroundShirasaki, M., Sifón, C., Miyatake, H., Lau, E. T., Zhang, Z., Bahcall, N. A., Battaglia, N., Devlin, M., Dunkley, J., Farahi, A., et al. (2024) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.110.103006 · Cited by 5
The doubloon models of dark haloes and galaxies
Evans, N. W., An, J., Bowden, A., & Williams, A. A. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv621 · Cited by 5
“Cosmological simulations suggest that dark halos are typically flattened and mildly oblate, with a ratio of long axis to short axis ofq = 0.8- 0.9 (see e.g., Abadi et al. 2010; Deason et al. 2011; Zemp et al. 2012).”
BackgroundInfluentialThe Response of the Inner Dark Matter Halo to Stellar Bars
Marostica, D. A., Machado, R. E. G., Athanassoula, E., & Manos, T. (2024) · Galaxies · doi:10.3390/galaxies12030027 · Cited by 5
DETECTING ADIABATIC CONTRACTION IN ROTATION CURVES
Puglielli, D. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/739/1/32 · Cited by 5
“…of four runs is implemented assuming three contraction prescriptions: the adiabatic contraction prescription of Blumenthal et al. (1986) which we label B, the modified adiabatic contraction prescription of Gnedin et al. (2004), labelled G, and the prescription of Abadi et al. (2010), labelled A.”
BackgroundMethodInfluentialLow Energy INTEGRAL Positrons from eXciting Dark MatterPreprint
Morris, R., & Weiner, N. (2011) · arXiv (Cornell University) · doi:10.48550/arxiv.1109.3747 · Cited by 5
Deciphering baryonic feedback from ACT tSZ galaxy clusters
Dalal, N., To, C., Hirata, C. M., Shin, T., Hilton, M., Pandey, S., & Bond, J. R. (2026) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2026/03/036 · Cited by 4
Pascale, R., Calura, F., Lupi, A., Rosdahl, J., Lacchin, E., Meneghetti, M., Nipoti, C., Vanzella, E., Vesperini, E., & Zanella, A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2749 · Cited by 4
PROBING THE GALACTIC POTENTIAL WITH NEXT-GENERATION OBSERVATIONS OF DISK STARS
Sumi, T., Johnston, K. V., Tremaine, S. D., Spergel, D. N., & Majewski, S. R. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/699/1/215 · Cited by 4
Halo Effect on Bar Rotation in Galaxies
Kondratyev, B. P., Киреева, Е. Н., Сергеевич, К. В., & Трубицына, Н. Г. (2022) · Astrophysics · doi:10.1007/s10511-022-09745-z · Cited by 3
The assembly of the Virgo cluster, traced by its galaxy haloes
Taylor, J. E., Shin, J., Ouellette, N. N.-Q., & Courteau, S. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1687 · Cited by 3
“Gnedin et al. (2004) generalized this result to eccentric orbits, predicting a somewhat weaker contraction, as did Abadi et al. (2010).”
ResultGamma Rays from Annihilations at the Galactic Center in a Physical Dark Matter Distribution
Lapi, A., Paggi, A., Cavaliere, A. G., Lionetto, A., Aldo Morselli, A., & Vitale, V. (2009) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/200913353/pdf · Cited by 4
A self-similar model of galaxy formation and dark halo relaxation
Velmani, P., & Paranjape, A. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/05/080 · Cited by 2
“The influence of galaxy formation on the dark halo is often interpreted as a process of (quasi-)adiabatic relaxation, where the orbits of dark matter particles respond to the condensation of baryons [19, 23, 29, 30].”
The Nearly Universal Disk Galaxy Rotation Curve
Patel, R., Arora, N., Courteau, S., Stone, C., Frosst, M., & Widrow, L. M. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad58bc · Cited by 2
“Much work along those lines has supported the halo contraction argument (e.g., Blumenthal et al. 1986; Abadi et al. 2010; Sawala et al. 2016), the halo expansion argument (e.g., Dutton et al. 2007; Governato et al. 2010; Macci`o et al. 2011; Chan et al. 2015), or both occurring at different epochs…”
BackgroundDynamics of the response of dark matter halo to galaxy evolution in IllustrisTNG
Velmani, P., & Paranjape, A. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/02/006 · Cited by 2
Lane, J., & Bovy, J. (2025) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staf294 · Cited by 2
Angular Momentum and the Validity of the Adiabatic Contraction AssumptionPreprint
Book, L. G., Brooks, A. M., Peter, A. H. G., Benson, A., & Governato, F. (2010) · arXiv (Cornell University) · Cited by 2
Galaxy–halo internal alignments across cosmic time
Marsengo-Colazo, V. A., Rodríguez, F., & Merchán, M. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202557043 · Cited by 1
Gravitational and mass distribution effects on stationary superwinds
Añorve-Zeferino, G. A. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1952 · Cited by 1
“Recent cosmological simulations carried out by Abadi et al. (2010) predict that dark matter haloes always contract as a result of galaxy formation.”
InfluentialDark Matter and Galaxy Formation
Primack, J. R. (2009) · CaltechAUTHORS (California Institute of Technology) · Cited by 1
Ruth Durrer, A., Parnovsky, S. L., CERN 1211 Geneva 23, S., & Parnowski, A. (2023) · Letters in High Energy Physics · doi:10.31526/lhep.2023.331 · Cited by 1
“which have, at present, achieved an impressive amount of detail [8, 9, 10, 11] or by simple analytical models, usually spherical collapse or secondary infall models [12, 13, 14, 15, 16].”
BackgroundCatastrophic dark matter particle capture
Ruth Durrer, A., & Parnovsky, S. L. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.107.063528 · Cited by 1
“Therefore, the non-linear regime of cosmological structure formation is usually treated either via N-body simulations, which have, at present, achieved an impressive amount of detail [6, 1, 8, 15] or by simple analytical models, usually spherical collapse or secondary infall models [16, 23, 12, 4].”
BackgroundEstimates dark halo parameters in S-galaxies
Butenko, M., Kuzmin, N., & Nichiporov, I. (2019) · Journal of Physics Conference Series · doi:10.1088/1742-6596/1400/2/022040
Spin Alignment in Analogues of The Local SheetPreprint
Conidis, G. J. (2016)
Влияние гало на вращение бара в галактиках
Кондратьев, Б. П., Киреева, Е. Н., Сергеевич, К. В., & Трубицына, Н. Г. (2022) · Astrophysics · doi:10.54503/0571-7132-2022.65.3-357
Zhu, H., & Gnedin, N. Y. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/aca1b3
N-body simulations: advantages and problems
Parnovsky, S. L. (2022) · Bulletin of Taras Shevchenko National University of Kyiv Astronomy · doi:10.17721/btsnua.2022.65.20-21
Strong gravitational lensing: Structure and evolution of galaxies
Verma, A., & Spiniello, C. (2025) · Elsevier eBooks · doi:10.1016/b978-0-443-21439-4.00110-3
The evolving role of astrophysical modelling in dark matter halo relaxation response
Velmani, P., & Paranjape, A. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/07/026
“The response of dark matter halo to galaxy formation has multiple aspects; we focus on the radial matter distribution relevant for mass profiles, rotation curves, etc. Early studies of individual haloes modelled this response as adiabatic relaxation of orbiting dark matter – 1 –”
InfluentialThe cusp-core problem in dwarf galaxies : new solutions
Boldrini, P. (2020) · theses.fr (ABES) · doi:10.70675/c317fdeczf52cz47cez89e9z4ade807675e4
Woudenberg, H. C. (2024) · Astronomy and Astrophysics · doi:10.5281/zenodo.13881902
Metadata
- Authors
- Abadi, M. G., Navarro, J. F., Fardal, M., Babul, A., & Steinmetz, M.
- Affiliations
- Consejo Nacional de Investigaciones Científicas y Técnicas (AR)
- University of Victoria (CA)
- University of Massachusetts Amherst (US)
- Leibniz Institute for Astrophysics Potsdam (DE)
- Corresponding author
- Abadi, Mario G.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2010-08-19
- Volume
- 407
- Issue
- 1
- Pages
- 435-446
- ISSN
- 0035-8711 (ISSN-L)
- OpenAlex
- W2159553024
- Cited by
- 237
- References
- 69
- Citations by year
- 2026: 1 · 2025: 7 · 2024: 15 · 2023: 12 · 2022: 14 · 2021: 11 · 2020: 10 · 2019: 14 · 2018: 12 · 2017: 6 · 2016: 17 · 2015: 11 · 2014: 20 · 2013: 13 · 2012: 31
- FWCI
- 14.30
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Conicet (publishedVersion, cc-by-nc-sa)
- arXiv (Cornell 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 › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- dark matter halos, galaxy formation, halo shape, halo mass profiles, radiative cooling, adiabatic contraction, galaxy assembly, luminosity function
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