The mass–concentration–redshift relation of cold dark matter haloes

By A. Ludlow, J. Navarro, R. Angulo, M. Boylan-Kolchin, Volker Springel, Carlos S. Frenk, Simon D. M. White. 2013

214 citations recorded by the source corpus.

We use the Millennium Simulation series to investigate the mass and redshift dependence of the concentration of equilibrium cold dark matter (CDM) halos. We extend earlier work on the relation between halo mass profiles and assembly histories to show how the latter may be used to predict concentrations for halos of all masses and at any redshift. Our results clarify the link between concentration and the ``collapse redshift'' of a halo as well as why concentration depends on mass and redshift solely through the dimensionless ``peak height'' mass parameter, $\nu(M,z)=\delta_{\rm crit}(z)/\sigma(M,z)$. We combine these results with analytic mass accretion histories to extrapolate the $c(M,z)$ relations to mass regimes difficult to reach through direct simulation. Our model predicts that, at given $z$, $c(M)$ should deviate systematically from a simple power law at high masses, where concentrations approach a constant value, and at low masses, where concentrations are substantially lower than expected from extrapolating published empirical fits. This correction may reduce the expected self-annihilation boost factor from substructure by about one order of magnitude. The model also reproduces the $c(M,z)$ dependence on cosmological parameters reported in earlier work, and thus provides a simple and robust account of the relation between cosmology and the mass-concentration-redshift relation of CDM halos.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/fb1d39a71a5798798830a728d3a08cc194e7579a

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Citations in the corpus

A UNIVERSAL MODEL FOR HALO CONCENTRATIONS (2014, background): “For this reason, both Prada et al. (2012) and Ludlow et al. (2014) have recently advocated modeling the c–ν relation rather than the c–”
The milky way total mass profile as inferred from Gaia DR2 (2019, background): “…Kafle et al. 2014; McMillan 2017; Monari et al. 2018; Lin & Li 2019), that is in tension with theoretical expectations based on cosmological simulations, which predict a mean concentration of ∼10 and a 68 percentile range of ∼[6, 10] (Ludlow et al. 2014; Hellwing et al. 2016; Klypin et al. 2016).”
Ultradiffuse galaxies: the high-spin tail of the abundant dwarf galaxy population (2016, methodology): “The concentration of halos follows the redshift dependent mass-concentration relation compiled by Gao et al. (2008), with a scatter of approximately 0.3 dex (e.g., Ludlow et al. 2014).”
The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation (2015, methodology): “As a result, various authors (Bullock et al. 2001; Wechsler et al. 2002; Zhao et al. 2003; Ludlow et al. 2014) have provided models that relate c to the halo mass history.”
An Accurate Physical Model for Halo Concentrations (2018, methodology): “M or c–ν relation (for partial exceptions see Ludlow et al. 2014; Okoli & Afshordi 2016).”
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 masses and density profiles of halos in a LCDM galaxy formation simulation (2014, background): “…between halo mass and concentration has been studied by many authors (e.g. AvilaReese et al. 1999; Jing 2000; Bullock et al. 2001; Eke, Navarro & Steinmetz 2001; Zhao et al. 2003; Neto et al. 2007; Duffy et al. 2008; Gao et al. 2008; Navarro et al. 2010; Dutton & Macciò 2014; Ludlow et al. 2014).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, methodology): “The combination of a strict criterion for the virial parameter and the lack of correction for the surface pressure produces an unwanted side effect in results of Ludlow et al. (2012, 2014).”
Halo and subhalo demographics with Planck cosmological parameters: Bolshoi–Planck and MultiDark–Planck simulations (2016, result): “…we analyze all dark matter halos and subhalos found by Rockstar, and do not just focus on those that satisfy some criteria for being “relaxed” or otherwise “good,” in contrast to some earlier studies of dark matter halo properties (e.g., Bett et al. 2007; Macciò et al. 2007; Ludlow et al. 2014).”
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measurement of the growth rate of structure from the anisotropic correlation function between redshift 0.8 and 2.2 (2018, methodology): “For each halo, we determine the concentration from the halo mass using an ad hoc parametrization of the data described in Ludlow et al. (2014).”
The influence of Sagittarius and the Large Magellanic Cloud on the stellar disc of the Milky Way Galaxy (2017, background): “Additionally, due to the scatter in the mass– concentration relation (Gao et al. 2008; Ludlow et al. 2014), we also consider two more progenitors that are twice as concentrated for the same given virial mass.”
The unexpected diversity of dwarf galaxy rotation curves (2015, methodology): “…and large cosmological simulations with excellent resolution have characterized conclusively the mass–concentration relation, its normalization, and scatter (see e.g. Neto et al. 2007; Duffy et al. 2008; Macciò, Dutton & van den Bosch 2008; Zhao et al. 2009; Prada et al. 2012; Ludlow et al. 2014).”