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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
Experimental — accuracy not yet measuredThe source backs part of the claim, not all of it — or backs it for a different population, condition or comparison.
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“This 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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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
Cited by
Sorted by citations
The 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
“When baryons are included, the halos become more spherical and evolve toward oblate at all radii but mostly in their inner parts (e.g., Kazantzidis et al. 2004, Bailin et al. 2005, Abadi et al. 2010).”
BackgroundUniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10
Behroozi, P., Wechsler, R. H., Hearin, A. P., & Conroy, C. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz1182 · Cited by 1,243
“Remaining effects of baryons on halo potential wells (e.g., making them less triaxial; Abadi et al. 2010) are more difficult to observe, and may require higher-order statistics such as three-point functions to capture.”
BackgroundFrom dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology
Guo, Q., White, S. D. M., Boylan-Kolchin, M., Lucia, G. D., Kauffmann, G., Lemson, G., Li, C., Springel, V., & Weinmann, S. M. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.18114.x · Cited by 1,205
“However, recent simulations suggest that this simple scheme overestimates the effect (e.g. Gnedin et al. 2004; Abadi et al. 2010).”
BackgroundKravtsov, A. V., & Borgani, S. (2012) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081811-125502 · Cited by 951
“At the same time, several recent studies showed that no single set of parameters of such simple models describes all objects that form in cosmological simulations equally well(Abadi et al. 2010; Gnedin et al. 2011; Gustafsson, Fairbairn & Sommer-Larsen 2006; Tisseraet al. 2010).”
BackgroundTHE TWO PHASES OF GALAXY FORMATION
Oser, L., Ostriker, J. P., Naab, T., Johansson, P. H., & Burkert, A. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/725/2/2312 · Cited by 840
“…expected from the effect of adiabatic contraction galaxies with significant in-situ star formation, i.e. more dissipation, live in more concentrated halos (Blumenthal et al. 1986; Dubinski 1994; Jesseit et al. 2002; Debattista et al. 2008; Gnedin et al. 2004; Abadi et al. 2010; Auger et al. 2010).”
Background
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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