The Power Spectrum Dependence of Dark Matter Halo Concentrations

By V. Eke, J. Navarro, Matthias Steinmetz. 2000

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High-resolution N-body simulations are used to examine the power spectrum dependence of the concentration of galaxy-sized dark matter halos. It is found that dark halo concentrations depend on the amplitude of mass fluctuations as well as on the ratio of power between small and virial mass scales. This finding is consistent with the original results of Navarro, Frenk, and White (NFW) and allows their model to be extended to include power spectra substantially different from cold dark matter (CDM). In particular, the single-parameter model presented here fits the concentration dependence on halo mass for truncated power spectra, such as those expected in the warm dark matter scenario, and predicts a stronger redshift dependence for the concentration of CDM halos than proposed by NFW. The latter conclusion confirms recent suggestions by Bullock and coworkers, although this new modeling differs from theirs in detail. These findings imply that observational limits on the concentration, such as those provided by estimates of the dark matter content within individual galaxies, may be used to constrain the amplitude of mass fluctuations on galactic and subgalactic scales. The constraints on ΛCDM models posed by the dark mass within the solar circle in the Milky Way and by the zero point of the Tully-Fisher relation are revisited, with the result that neither data set is clearly incompatible with the "concordance" (Ω0 = 0.3, Λ0 = 0.7, σ8 = 0.9) ΛCDM cosmogony. This conclusion differs from that reached recently by Navarro and Steinmetz, a disagreement that can be traced to inconsistencies in the normalization of the ΛCDM power spectrum used in that work.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/31de5ae51c776aa8f96963c85f03c54203a87167

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Citations in the corpus

The haloes of bright satellite galaxies in a warm dark matter universe (2011, background): “Concentrations typically reflect the epoch at which the halo formed (Navarro et al. 1996b, 1997; Eke et al. 2001).”
Damped Lyman α systems in galaxy formation simulations (2008, background): “It should be noted, however, that in common with other galaxy formation simulations, the mass in the bulge component of the G07 galaxies is overestimated (see also Eke et al. 2001).”
Bar-driven Dark Halo Evolution: A Resolution of the Cusp-Core Controversy (2001, background): “…of the dark particle from cold to warm to reduce the small scale power, i.e. warm dark matter (Hogan and Dalcanton 2000; Coĺin et al. 2000; Eke et al. 2001; Avila-Reese et al. 2001; Bode et al. 2001), while others altered the shape of the spectrum at small scales by changing inflation…”
Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology (2008, background): “Simulations have shown that these two parameters are correlated, with the average concentration of a halo being a weakly decreasing function of mass (e.g. NFW; Bullock et al. 2001; Eke et al. 2001, hereafter ENS; Shaw et al. 2006; Maccio et al. 2007).”
The Metamorphosis of Tidally Stirred Dwarf Galaxies (2001, background): “In fact, in CDM cosmogonies, the average central density of halos on the mass scale of dwarfs is higher than that of our LSB models (the GR 8 model being an exception), the latter being closer to the typical central density of small halos in WDM models (Bode et al. 2001 ; Eke et al. 2001).”
Halo Models of Large Scale Structure (2002, positive): “|( ln 13.0 * 2 ln 2 2 ≈⎥ ⎦ ⎤ ⎢ ⎣ ⎡ + = ⎥ ⎦ ⎤ ⎢ ⎣ ⎡ −= − c cc zm m z zmc zmcccddczmcp σ σπσ more massive halo less concentrated (Eke et al., 2001) (Sheth et al., 2002)”
Tracing cosmic evolution with clusters of galaxies (2004, background): “Also, lower-mass objects tend to have higher halo concentrations because they formed earlier in time, when the overall density of the universe was greater sNavarro et al., 1997; Bullock et al., 2001; Eke et al., 2001d.”
The mass profile and accretion history of cold dark matter haloes (2013, background): “…on mass, was originally linked to halo collapse time (Navarro et al. 1997), but attempts to reproduce the simulation results with simple prescriptions based on that proposal have met with limited success (Bullock et al. 2001; Eke et al. 2001; Neto et al. 2007; Macciò et al. 2008; Gao et al. 2008).”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “In many studies it has been found that halos of a given mass exhibit a well-defined characteristic concentration (Navarro et al., 1997; Eke et al., 2001; Bullock et al., 2001; Neto et al., 2007; Gao et al., 2007), or in other words, that the radius rmax at which the circular velocity peaks is…”