Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles

By A. Dutton, A. Macciò. 2014

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We present the evolution of the structure of relaxed cold dark matter haloes in the cosmology from the Planck satellite. Our simulations cover 5 decades in halo mass, from dwarf galaxies to galaxy clusters. Due to the increased matter density and power spectrum normalization the concentration mass relation in the Planck cosmology has a 20 percent higher normalization at redshift z=0 compared to WMAP cosmology. We confirm that CDM haloes are better described by the Einasto profile; for example, at scales near galaxy half-light radii CDM haloes have significantly steeper density profiles than implied by NFW fits. There is a scatter of 0.2 dex in the Einasto shape parameter at fixed halo mass, adding further to the diversity of CDM halo profiles. The evolution of the concentration mass relation in our simulations is not reproduced by any of the analytic models in the literature. We thus provide a simple fitting formula that accurately describes the evolution between redshifts z=5 to z=0 for both NFW and Einasto fits. Finally, the observed concentrations and halo masses of spiral galaxies, groups and clusters of galaxies at low redshifts are in good agreement with our simulations, suggesting only mild halo response to galaxy formation on these scales.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/a4cbdc923d961f4dafc69704a32ea84f7f10a6bd

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Citations in the corpus

A UNIVERSAL MODEL FOR HALO CONCENTRATIONS (2014, background): “Our results (see also Dutton & Macciò 2014) show that there is no well-defined floor in the concentration values: halos that form from the collapse of perturbations with a steep power spectrum have concentrations much smaller than the floor value adopted by Zhao et al. (2009).”
The Canadian Cluster Comparison Project: detailed study of systematics and updated weak lensing masses (2015, methodology): “Dutton & Macciò (2014) present fitting functions for the mass–concentration relation for this cosmology, which we use when we estimate cluster masses (cf. Table 2).”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, background): “…are well fit by the NFW profile (equation 1) at all redshifts down to a few per cent of the virial radius (Navarro et al. 1997, 2004; Bullock et al. 2001; Eke et al. 2001; Shaw et al. 2006; Macciò et al. 2007; Neto et al. 2007; Duffy et al. 2008; Ludlow et al. 2013; Dutton & Macciò 2014).”
The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation (2015, methodology): “Dutton & Macciò (2014) found that the c–”
Characterization of subhalo structural properties and implications for dark matter annihilation signals (2016, background): “…intrinsic, irreducible scatter is expected on the concentration of DM halos of the same mass (Jing 2000; Bullock et al. 2001; Macciò et al. 2007; Neto et al. 2007; Macciò et al. 2008; Dutton & Macciò 2014), which mainly reflects their slightly different formation epochs (Wechsler et al. 2002).”
The universality of the virial halo mass function and models for non-universality of other halo definitions (2015, background): “Some of the discrepancy may be caused by the fact that not all haloes follow NFW profiles all the way down to the very center (Einasto 1965; Retana-Montenegro et al. 2012; Ludlow et al. 2013; Dutton & Macciò 2014).”
Mass and shape of the Milky Way’s dark matter halo with globular clusters from Gaia and Hubble (2018, methodology): “…of the mass of the Galaxy within 20 kpc to the virial radius2, assuming a concentration-mass relation as calibrated from numerical simulations (Dutton & Macciò 2014), we get the following final estimate of the total mass of the Galaxy, Mvir = 1.3 ± 0.3 × 1012M (13) and hence a virial radius…”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, methodology): “Dutton & Macciò (2014) did not find the upturn when they fit the Einasto profile to dark matter density profiles.”
NIHAO project – I. Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations (2015, methodology): “The simulated galaxies were selected from two cosmological boxes of sides 60 and 20 Mpc/h from Dutton & Macciò (2014), as well as a new simulation of size 15 Mpc/h with 4003 particles.”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “Among them {lgM1h , lgM0∗ , β, δ, γ} describe the mean SHMR, 3 However, see Gao et al. (2008) and Dutton & Macciò (2014) regarding potentially better “universality” when using the Einasto (1965) profile.”
COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, methodology): “Most works rely on NFW-based concentrations, i.e. fitting halo profiles with the NFW form to derive rs, but other parameterizations exist (e.g., Klypin et al. 2011, Prada et al. 2012; see Dutton & Macciò 2014 for a comparison with Einasto-based concentrations).”
The hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2 (2018, methodology): “In the top-left panel, dashed lines indicate the halo mass–concentration relations that describe field haloes at redshifts z = 0, 1, . . . , 6 (right to left), derived from the cosmological N-body simulations of Dutton & Macciò (2014).”
Dark Matter Substructure in Numerical Simulations: A Tale of Discreteness Noise, Runaway Instabilities, and Artificial Disruption (2018, neutral): “1 (e.g., Dutton & Macciò 2014).”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, methodology): “As an approximation for the potential, we assume that each halo follows an NFW profile with a concentration parameter given by Dutton & Macciò (2014).”
THE SMALL SCATTER OF THE BARYONIC TULLY–FISHER RELATION (2015, neutral): “The mass-concentration relation has a well-established scatter of 0.11 dex from N-body simulations (Dutton & Macciò 2014), driving scatter on fV.”
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.”
The mass–concentration–redshift relation of cold and warm dark matter haloes (2016, methodology): “Solid coloured lines assume an Einasto profiles with α = 0.18; dashed lines assume an NFW profile, and the shaded region highlights the range of c expected given the (redshift dependent) scatter in α reported by Dutton & Macciò (2014).”