Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology

By Alan R. Duffy, Joop Schaye, S. Kay, Claudio Dalla Vecchia, J. B. C. F. Astrophysics, L. Observatory. 2008

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We use a combination of three large N-body simulations to investigate the dependence of dark matter halo concentrations on halo mass and redshift in the Wilkinson Microwave Anisotropy Probe year 5 (WMAP5) cosmology. The median relation between concentration and mass is adequately described by a power law for halo masses in the range 1011–1015 h−1 M⊙ and redshifts z < 2, regardless of whether the halo density profiles are fitted using Navarro, Frenk & White or Einasto profiles. Compared with recent analyses of the Millennium Simulation, which uses a value of σ8 that is higher than allowed by WMAP5, z= 0 halo concentrations are reduced by factors ranging from 23 per cent at 1011 h−1 M⊙ to 16 per cent at 1014 h−1 M⊙. The predicted concentrations are much lower than inferred from X-ray observations of groups and clusters.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/c2b79d9e076acb2a3f7ceb3a6cebe49f126e191e

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SEVEN-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: COSMOLOGICAL INTERPRETATION (2010, methodology): “Recently, Duffy et al. (2008) ran larg e N -body simulations with the WMAP 5-year cosmological parameters to find a more accurate fitting formula for the concentration parameter: cduffy = 7.85 (1 + z)0.71 ( Mvir 2 × 1012 h−1 M⊙ )−0.081 = 5.72 (1 + z)0.71 ( Mvir 1014 h−1 M⊙ )−0.081 .”
Quantifying the effect of baryon physics on weak lensing tomography (2011, methodology): “We use the mass-concentration relation derived by Duffy et al. (2008).”
Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles (2014, background): “…et al. 2007, 2008; Muñoz-Cuartas et al. 2011), as well as numerous studies in the literature (e.g., Navarro, Frenk & White 1996, 1997; Bullock et al. 2001; Eke et al. 2001; Zhao et al. 2003, 2009; Duffy et al. 2008; Gao et al. 2008; Klypin et al. 2011; Prada et al. 2012; Ludlow et al. 2013).”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, background): “Not unexpectedly, given the sensitivity of the concentration to changes in the cosmological parameters, the values for the fit we obtain for the DMO simulation are significantly different from those reported by Neto et al. (2007), Macciò et al. (2007), and Duffy et al. (2008).”
The mass–concentration–redshift relation of cold dark matter haloes (2013, result): “10, where we compare the predictions of our model with the fitting formulae proposed by Duffy et al. (2008), Macciò et al. (2008) and Prada et al. (2012) for the WMAP5, WMAP3 and WMAP7 cosmologies, respectively.”
THE ATACAMA COSMOLOGY TELESCOPE: ACT-CL J0102−4915 “EL GORDO,” A MASSIVE MERGING CLUSTER AT REDSHIFT 0.87 (2011, methodology): “This conversion factor was derived using a Navarro, Frenk, & White (1997) mass profile (hereafter NFW) and the concentrationmass relation, c(M,z), from simulations (Duffy et al. 2008) at z = 0.87 for the mass of the cluster.”
The relation between velocity dispersion and mass in simulated clusters of galaxies: dependence on the tracer and the baryonic physics (2013, background): “Given that the real, simulated halos are not perfect NFW spheres, and that a halo concentration depends on its mass and redshift (e.g. Duffy et al. 2008; Gao et al. 2008), the real values of A1D and α can be different, and need to be evaluated from the data.”
New Multiply-Lensed Galaxies Identified in ACS/NIC3 Observations of Cl0024+1654, Using an Improved Mass Model (2009, background): “This value is significantly larger than theoretically expected (cvir ' 5) for the standard ΛCDM model (Bullock et al. 2001, Neto et al. 2007, Duffy et al. 2008), even after accounting for expected projection bias (Oguri et al. 2005, Hennawi et al. 2007, Corless, King & Clowe 2008).”
Cluster Cosmology Constraints from the 2500 deg2 SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope (2018, methodology): “In addition, we present the mass M200c for each system, assuming the concentration–mass relation from Duffy et al. (2008).”
ON THE SHOULDERS OF GIANTS: PROPERTIES OF THE STELLAR HALO AND THE MILKY WAY MASS DISTRIBUTION (2014, background): “Simulated virialized halos inΛCDM cosmology, in general predict an inversely proportional relation between their mass and concentration (e.g. Bullock et al. 2001; Macciò et al. 2007; Duffy et al. 2008; King & Mead 2011).”
hmcode-2020: improved modelling of non-linear cosmological power spectra with baryonic feedback (2020, methodology): “…mass function and halo bias4 from Sheth & Tormen (1999)5 with the linear collapse threshold calculated using the fitting formula of Nakamura & Suto (1997); we take Navarro et al. (NFW; 1997) halo profiles with a concentration, c = rv/rs appropriate for virial haloes taken from Duffy et al. (2008).”
An Accurate Physical Model for Halo Concentrations (2018, background): “…typically with power laws or other 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…”
KiDS-450: The tomographic weak lensing power spectrum and constraints on cosmological parameters (2017, methodology): “For that we further assume an NFW halo profile (Navarro, Frenk & White 1997) with the concentration–mass relation by Duffy et al. (2008) and use the analytical form of its Fourier transform as given in Scoccimarro et al. (2001).”
The unexpected diversity of dwarf galaxy rotation curves (2015, background): “…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).”
Baryon impact on the halo mass function: Fitting formulae and implications for cluster cosmology (2015, methodology): “We use the parametrizations by Navarro, Frenk & White (1997) and Duffy et al. (2008) and establish an analytic fit for M500c/M200m.”
Galactic Searches for Dark Matter (2012, background): “For the updated values of cosmological parameters and for halo masses above approximately 1011 M , the concentration-mass relation for the Einasto profile is (Duffy et al., 2008) cvir(Mvir,z) = 8.82 (1 + z)0.87 ( Mvir 2× 1012h−1M )−0.106 .”
The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost (2013, background): “Most of the existing c(M) median relations proposed in the literature were derived from well resolved simulations in the halo mass range from 1010 – 1015h−1M⊙, e.g., B01, Hennawi et al. (2007); Neto et al. (2007); Duffy et al. (2008), M08, Muñoz-Cuartas et al. (2011), P12.”
COLOSSUS: A Python Toolkit for Cosmology, Large-scale Structure, and Dark Matter Halos (2017, neutral): “First, the c-M relation is reasonably well described by a power law for a given redshift and cosmology, and within a certain range of halo mass (Duffy et al. 2008; Klypin et al. 2011; Dutton & Macciò 2014; Klypin et al. 2016; Child et al. 2018).”