The mass profile and accretion history of cold dark matter haloes

Ludlow, Aaron D.; Navarro, Julio F.; Boylan-Kolchin, Michael; Bett, Philip E.; Angulo, Raúl E.; Li, Ming; White, Simon D. M.; Frenk, Carlos S.; Springel, Volker

doi:10.1093/mnras/stt526

Cited by 219 publications

(262 citation statements)

References 47 publications

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“…If the residual acceleration, asphericity and small scale structures of the ICM, which are the most likely sources of the scatter, are better understood in the future, then knowledge of nonthermal pressure in individual clusters will be very helpful in getting accurate individual masses. The mass accretion history and the non-thermal pressure for individual clusters may also be obtainable by exploiting the connection between the mass density profile and the mass accretion history (Ludlow et al 2013;Diemer & Kravtsov 2014). Namely, first compute a mass profile from a cluster without correcting for non-thermal pressure, and then compute the mass accretion history from the mass profile, compute non-thermal pressure, and recompute the mass profile.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Analytical model for non-thermal pressure in galaxy clusters – III. Removing the hydrostatic mass bias

Shi

Komatsu

Nagai

et al. 2015

Mon. Not. R. Astron. Soc.

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Non-thermal pressure in galaxy clusters leads to underestimation of the mass of galaxy clusters based on hydrostatic equilibrium with thermal gas pressure. This occurs even for dynamically relaxed clusters that are used for calibrating the mass-observable scaling relations. We show that the analytical model for non-thermal pressure developed in Shi & Komatsu (2014) can correct for this so-called 'hydrostatic mass bias', if most of the non-thermal pressure comes from bulk and turbulent motions of gas in the intracluster medium. Our correction works for the sample average irrespective of the mass estimation method, or the dynamical state of the clusters. This makes it possible to correct for the bias in the hydrostatic mass estimates from X-ray surface brightness and the Sunyaev-Zel'dovich observations that will be available for clusters in a wide range of redshifts and dynamical states.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Analytical model for non-thermal pressure in galaxy clusters – III. Removing the hydrostatic mass bias

Shi

Komatsu

Nagai

et al. 2015

Mon. Not. R. Astron. Soc.

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“…With the advent of simulations with increasingly higher resolution, the universality of the NFW density profile has been questioned (see e.g. Navarro et al 2004;Vogelsberger et al 2011;Ludlow et al 2013). While the self-similarity of the density profiles of DM-only haloes may not hold as well as initially thought, another physical parameter appears to have a quasiuniversal radial profile, the pseudo phase-space density (PPSD) Q(r) = ρ/σ 3 , where ρ is the total matter density profile and σ the 3D velocity dispersion of the tracers of the gravitational potential (Taylor & Navarro 2001;Ludlow et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Munari

Biviano

Mamon

2014

A&A

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Aims. We aim to compute the mass and velocity anisotropy profiles of Abell 2142 and, from there, the pseudo phase-space density profile Q(r) and the density slope − velocity anisotropy β − γ relation, and then to compare them with theoretical expectations. Methods. The mass profiles were obtained by using three techniques based on member galaxy kinematics, namely the caustic method, the method of dispersion-kurtosis, and MAMPOSSt. Through the inversion of the Jeans equation, it was possible to compute the velocity anisotropy profiles. Results. The mass profiles, as well as the virial values of mass and radius, computed with the different techniques agree with one another and with the estimates coming from X-ray and weak lensing studies. A combined mass profile is obtained by averaging the lensing, X-ray, and kinematics determinations. The cluster mass profile is well fitted by an NFW profile with c = 4.0 ± 0.5. The population of red and blue galaxies appear to have a different velocity anisotropy configuration, since red galaxies are almost isotropic, while blue galaxies are radially anisotropic, with a weak dependence on radius. The Q(r) profile for the red galaxy population agrees with the theoretical results found in cosmological simulations, suggesting that any bias, relative to the dark matter particles, in velocity dispersion of the red component is independent of radius. The β − γ relation for red galaxies matches the theoretical relation only in the inner region. The deviations might be due to the use of galaxies as tracers of the gravitational potential, unlike the non-collisional tracer used in the theoretical relation.

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“…Early theoretical discussions of the cusp-core problem devoted considerable attention to the predicted central slope of the density profiles and to the effects of finite numerical resolution and cosmological parameter choices on the simulation predictions [a recent state-of-the-art discussion is provided by Ludlow et al (14)]. However, the details of the inner profile shape are not essential to the conflict; the basic problem is that CDM predicts too much dark matter in the central few kpc of typical galaxies, and the tension is evident at scales where v c ðrÞ has risen to ∼ 1=2 of its asymptotic value (e.g., refs.…”

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confidence: 99%

Cold dark matter: Controversies on small scales

Weinberg

Bullock

Governato

et al. 2015

Proc. Natl. Acad. Sci. U.S.A.

421

346

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The cold dark matter (CDM) cosmological model has been remarkably successful in explaining cosmic structure over an enormous span of redshift, but it has faced persistent challenges from observations that probe the innermost regions of dark matter halos and the properties of the Milky Way's dwarf galaxy satellites. We review the current observational and theoretical status of these "small-scale controversies." Cosmological simulations that incorporate only gravity and collisionless CDM predict halos with abundant substructure and central densities that are too high to match constraints from galaxy dynamics. The solution could lie in baryonic physics: Recent numerical simulations and analytical models suggest that gravitational potential fluctuations tied to efficient supernova feedback can flatten the central cusps of halos in massive galaxies, and a combination of feedback and low star formation efficiency could explain why most of the dark matter subhalos orbiting the Milky Way do not host visible galaxies. However, it is not clear that this solution can work in the lowest mass galaxies, where discrepancies are observed. Alternatively, the small-scale conflicts could be evidence of more complex physics in the dark sector itself. For example, elastic scattering from strong dark matter self-interactions can alter predicted halo mass profiles, leading to good agreement with observations across a wide range of galaxy mass. Gravitational lensing and dynamical perturbations of tidal streams in the stellar halo provide evidence for an abundant population of low-mass subhalos in accord with CDM predictions. These observational approaches will get more powerful over the next few years.dark matter | cosmology | galaxy formation T he cold dark matter (CDM) hypothesis-that dark matter consists of a weakly interacting particle whose velocity dispersion in the early universe was too small to erase structure on a galactic or subgalactic scale-emerged in the early 1980s and quickly became a central element of the theory of cosmic structure formation. Influential early papers include Peebles' calculation of cosmic microwave background (CMB) anisotropies and the matter power spectrum (1), discussions of galaxy formation with particle dark matter by Bond et al. (2) and Blumenthal et al. (3,4), and Davis et al.'s (5) numerical simulations of galaxy clustering. By the mid-1990s, the simplest CDM model with scale-invariant primordial fluctuations and a critical matter density of ðΩ m = 1Þ had run afoul of multiple lines of observational evidence, including the shape of the galaxy power spectrum, estimates of the mean matter density from galaxy clusters and galaxy motions, the age of the universe inferred from estimates of the Hubble constant, and the amplitude of matter clustering extrapolated forward from the fluctuations measured in the CMB. Many variants on "canonical" CDM were proposed to address these challenges, and by the turn of the century, the combination of supernova evidence for cosmic acceleration and CMB evidence for ...

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The mass profile and accretion history of cold dark matter haloes

Cited by 219 publications

References 47 publications

Analytical model for non-thermal pressure in galaxy clusters – III. Removing the hydrostatic mass bias

Analytical model for non-thermal pressure in galaxy clusters – III. Removing the hydrostatic mass bias

Mass, velocity anisotropy, and pseudo phase-space density profiles of Abell 2142

Cold dark matter: Controversies on small scales

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