Concentration, spin and shape of dark matter haloes as a function of the cosmological model: WMAP1, WMAP3 and WMAP5 results

By A. Macciò, A. Dutton, F. V. D. Bosch. 2008

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We investigate the effects of changes in the cosmological parameters between the Wilkinson Microwave Anisotropy Probe (WMAP) 1st, 3rd and 5th year results on the structure of dark matter haloes. We use a set of simulations that cover five decades in halo mass ranging from the scales of dwarf galaxies (V c ≈ 30 km s -1 ) to clusters of galaxies (V c ≈ 1000 km s -1 ). We find that the concentration mass relation is a power law in all three cosmologies. However, the slope is shallower and the zero-point is lower moving from WMAP1 to WMAP5 to WMAP3. For haloes of mass log M 200 /[h -1 M ⊙ ] = 10, 12 and 14 the differences in the concentration parameter between WMAP1 and WMAP3 are a factor of 1.55,1.41 and 1.29, respectively. As we show, this brings the central densities of dark matter haloes in good agreement with the central densities of dwarf and low surface brightness galaxies inferred from their rotation curves, for both the WMAP3 and WMAP5 cosmologies. We also show that none of the existing toy models for the concentration-mass relation can reproduce our simulation results over the entire range of masses probed. In particular, the model of Bullock et al. fails at the higher mass end (M ≥ 10 13 h-1 M ⊙ ), while the NFW model of Navarro, Frenk and White fails dramatically at the low-mass end (M ≤ 10 12 h -1 M ⊙ ). We present a new model, based on a simple modification of that of Bullock et al., which reproduces the concentration-mass relations in our simulations over the entire range of masses probed (10 10 ≤ M ≤ 10 15 h -1 M ⊙ ). Haloes in the WMAP3 cosmology (at a fixed mass) are more flatted compared to the WMAP1 cosmology, with a medium to long axis ration reduced by ≈ 0 per cent. Finally, we show that the distribution of halo spin parameters is the same for all three cosmologies.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/65cc0fdba0207c1caa3cf09c3e094dc6c8647329

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Citations in the corpus

Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles (2010, background): “…results has been the existence of power law relationships in the phase-space density of haloes across several decades in radius (Taylor & Navarro 2001) and the halo concentrationmass relation over five decades in mass (Bullock et al. 2001; Neto et al. 2007; Macciò et al. 2008; Duffy et al. 2008).”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, background): “Previous studies have shown that average halo concentrations decrease weakly with halo mass – c ∝M−0.1 – with a fairly large scatter at fixed mass, σ(log10 M) ≈ 0.1−0.14 (Navarro et al. 1997; Jing 2000; Bullock et al. 2001b; Neto et al. 2007; Gao et al. 2008; Macciò et al. 2008; Zhao et al. 2009).”
The RAVE survey : the Galactic escape speed and the mass of the Milky Way (2013, methodology): “This scatter is reasonably well fitted by a log-normal distribution with σlog c = 0.11 (e.g. Macciò et al. 2008; Neto et al. 2007).”
Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation (2014, unknown): “Following Choi et al. (2010), we used the Two degree Field Galaxy Redshift Survey (2dFGRS, Colless et al., 2001, 2003), the Two Micron All Sky Survey (2MASS, Jarrett et al., 2003; Skrutskie et al., 2006) Redshift Survey (2MRS, Huchra et al., 2012), and the Third Reference Catalogue of Bright Galaxie”
THE VELOCITY WIDTH FUNCTION OF GALAXIES FROM THE 40% ALFALFA SURVEY: SHEDDING LIGHT ON THE COLD DARK MATTER OVERABUNDANCE PROBLEM (2011, background): “In order to display their results in Figure14, (red & blue hatched regions) we have transformed virial velocities into halo maximum rotational velocities assuming average halo concentrations (Macciò et al. 2008).”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “…(e.g., Warren et al. 1992; Jing & Suto 2002; Bailin & Steinmetz 2005; Kasun & Evrard 2005; Allgood et al. 2006; Shaw et al. 2006; Bett et al. 2007; Macciò et al. 2007, 2008) can bias a spherically-symmetric model fit of the reduced tangential shear profile and lead to errors of≈±30− 50% in the…”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:a large sample of mock galaxy catalogues (2012, background): “The scatter of the mass-concentration is not dependent on cosmological parameters (Maccio et al. 2008).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, background): “…on mass, redshift, and cosmological parameters – has been the subject of extensive analysis for a long period of time (Navarro et al. 1997; Jing 2000; Bullock et al. 2001; Neto et al. 2007; Gao et al. 2008; Macciò et al. 2008; Klypin et al. 2011; Prada et al. 2012; Dutton & Macciò 2014).”
An Accurate Physical Model for Halo Concentrations (2018, background): “…simple functions (Avila-Reese et al. 1999; Jing 2000; Colín et al. 2004; Dolag et al. 2004; Neto et al. 2007; Duffy et al. 2008; Gao et al. 2008; Macciò et al. 2008; Klypin et al. 2011; Muñoz-Cuartas et al. 2011; Bhattacharya et al. 2013; Dutton & Macciò 2014; Heitmann et al. 2015; Klypin et…”
DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION (2010, background): “For Mvir = 10 15h−1M⊙ our results give c = 5.7 while Macciò et al. (2008) predict c = 4.0 – a 40% difference.”
NIHAO - XI. Formation of ultra-diffuse galaxies by outflows (2016, result): “This result is in contrast with the derived mass of two other UDGs: using the abundance of their globular clusters, 1 The Macciò et al. (2008) c-M relation was used, giving up to 30% lower concentration than the Planck one used here, allowing a fit into a larger halo. c© 2010 The Authors ar X iv…”
The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation (2015, background): “M relations from Bullock et al. (2001) and Macciò et al. (2008) to their simulation outputs, and concluded that extrapolating simple power-law approximations to typical microhalo scales results in an overestimation of c by up to a factor of 10 at low-z.”
Luminosity function and radial distribution of Milky Way satellites in a ΛCDM Universe (2009, unknown): “We include in the halo catalogue all the haloes with more than 100 particles (see Macciò et al. 2007, 2008 for further details on our halo finding algorithm).”
Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles (2014, methodology): “As found by Macciò et al. (2008), for this model to reproduce the simulations exactly, the parameter K needs to vary slightly (by a few percent) for different cosmologies.”
Accurate masses for dispersion-supported galaxies (2009, methodology): “We have used the median concentration (c = 11) predicted by the Bullock et al. (2001) mass-concentration model updated by Macciò et al. (2008) for WMAP5 ΛCDM parameters.”