The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation

By Camila A Correa, J. Stuart B. Wyithe, Joop Schaye, Alan R. Duffy. 2015

192 citations recorded by the source corpus.

We present a semi-analytic, physically motivated model for dark matter halo concentration as a function of halo mass and redshift. The semi-analytic model is intimately based on hierarchical structure formation. It uses an analytic model for the halo mass accretion history, based on extended Press Schechter (EPS) theory, and an empirical relation between concentration and an appropriate definition of formation time obtained through fits to the results of numerical simulations. The resulting concentration-mass relations are tested against the simulations and do not exhibit an upturn at high masses or high redshifts as claimed by recent works. Because our semi-analytic model is based on EPS theory, it can be applied to wide ranges in mass, redshift and cosmology. We predict a change of slope in the z = 0 concentration-mass relation at a mass scale of 10 11 M⊙, that is caused by the varying power in the density perturbations. We provide best-fitting expressions of the c M relations as well as numerical routines†. We investigate how halo mass accretion histories affect the evolution of concentrations, finding that the decrease in the accretion rate during the dark energy epoch, produced by the accelerated expansion of the Universe, allows dark matter halos to virialize, relax and contract, and thus concentrations to grow. We also analyzed how the concentration-mass relation predicted by this work affects the power produced by dark matter annihilation.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/4a0b188175ebfd94bfb8777ca27ec0fb6c145f0f

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Citations in the corpus

The formation and assembly history of the Milky Way revealed by its globular cluster population (2018, methodology): “For comparison, the application of the extended Press-Schechter formalism to the Planck cosmology adopted in this work shows that haloes of mass M200 = 1012 M reach {25, 50} per cent of their presentday mass at redshift z = {2.3, 1.2} (Correa et al. 2015).”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “A number of recent studies (Prada et al. 2006; Diemand et al. 2007; Cuesta et al. 2008; Diemer et al. 2013; Diemer & Kravtsov 2014; Zemp 2014; Correa et al. 2015) have pointed out that the inner density profiles of low-mass, galaxy-sized halos evolve very little at z 1 .”
What does the Bullet Cluster tell us about Self-Interacting Dark Matter? (2016, background): “…the main halo derived from weak lensing would place this halo well below the concentration–mass relation derived from observations of galaxy clusters (Merten et al. 2015), or from numerical (Prada et al. 2012; Dutton & Macciò 2014; Diemer & Kravtsov 2015) or analytical (Correa et al. 2015) work.”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, background): “(B18) We can generalize the above function to characterize the halo mass growth of any progenitor at any redshift z0 by moving the origin from z to z → z − z0, (see e.g., Correa et al. 2015).”
An Accurate Physical Model for Halo Concentrations (2018, methodology): “On the other hand, removing the upturn by aggressively cutting out unrelaxed halos necessarily leads to a bias toward dynamically older systems and thus higher concentrations (Ludlow et al. 2012; Prada et al. 2012; Correa et al. 2015c; Angel et al. 2016; Klypin et al. 2016; Child et al. 2018).”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, unknown): “…relations, c(M), have been proposed in the literature (see, e.g., Bullock et al. (2001); Hennawi et al. (2007); Neto et al. (2007); Duffy et al. (2008); Macciò et al. (2008); Muñoz Cuartas et al. (2011); Prada et al. (2012); Ludlow et al. (2014); Diemer & Kravtsov (2014); Correa et al. (2015)).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, result): “Adapted from Correa et al. (2015) with permission. difficulty of measuring a star’s age continues to hamper progress in Galactic studies, but this stumbling block will be partly offset by the ESA Gaia astrometric survey already under way.”
hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback (2020, methodology): “While this works well for our purposes, as demonstrated in Section 3, it may be preferable to update the relations to those presented in Correa et al. (2015), Ludlow et al. (2016) or Diemer & Joyce (2019), where the concentration is tied to the halo mass-accretion history.”
The mass–concentration–redshift relation of cold and warm dark matter haloes (2016, methodology): “…of algorithms accurately reproduce not only the evolution of the main progenitor halo (e.g. van den Bosch 2002; Jiang & van den Bosch 2014; Correa et al. 2015a,b), but the entire hierarchy of progenitors for both CDM (e.g. Parkinson, Cole & Helly 2008) and WDM (e.g. Benson et al. 2013)…”
COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, background): “Some noteworthy models are not implemented in Colossus, most commonly because they are not based on simple analytical expressions and thus demand significant computation (e.g. Eke et al. 2001; Zhao et al. 2009; Correa et al. 2015).”