The power spectrum of SUSY-CDM on subgalactic scales

By A. Green, S. Hofmann, D. Schwarz. 2003

168 citations recorded by the source corpus.

ABSTRACT The formation of large scale structure is independent of the nature of the cold darkmatter (CDM), however the fate of very small scale inhomogeneities depends on themicro-physics of the CDM particles. We investigate the matter power spectrum forscales that enter the Hubble radius well before matter-radiation equality, and followits evolution until the time when the ﬁrst inhomogeneities become non-linear. Ourfocus lies on weakly interacting massive particles (WIMPs), and as a concrete exam-ple we analyze the case when the lightest supersymmetric particle is a bino. We showthat collisional damping and free-streaming of WIMPs lead to a matter power spec-trum with a sharp cut-oﬀ at about 10 −6 M ⊙ and a maximum close to that cut-oﬀ. Wealso calculate the transfer function for the growth of the inhomogeneities in the lin-ear regime. These three eﬀects (collisional damping, free-streaming and gravitationalgrowth) are combined to provide a WMAP normalized primordial CDM power spec-trum, which could serve as an input for high resolution CDM simulations. The smallestinhomogeneities typically enter the non-linear regime at a redshift of about 60.Key words: cosmology: theory – dark matter – early Universe

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/3c94761215ad6fba4e449b9010bddd6c75e86577

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Citations in the corpus

The first WIMPy halos (2005, unknown): “Keywords: dark matter, cosmological perturbation theory ArXiv ePrint: astro-ph/0503387 Contents”
Gravitational probes of dark matter physics (2017, methodology): “elic, the power spectrum is exponentially suppressed once the dark matter kinetically decouples from the Standard Model particle bath. This occurs at a temperature T kd, with the approximate relation [172, 173, 174, 175] M halo ˘ 10 1 M T kdg 1=4 e 50 MeV ! 3 (30) 19 where g e is the number of eecti”
Galactic Searches for Dark Matter (2012, background): “For standard cold dark matter particles with mass around the weak scale and freeze-out temperatures & GeV, the minimum mass subhalo is predicted to be somewhere in the range of an Earth mass (Green et al., 2004; Loeb and Zaldarriaga, 2005; Profumo et al., 2006; Martinez et al., 2009).”
The Aquarius Project: the subhaloes of galactic haloes (2008, background): “Depending on the specific particle physics model, this cut-off lies around an Earth mass, at ∼ 10−6 M⊙, but could be as low as 10−12 M⊙ in certain scenarios (Hofmann et al., 2001; Green et al., 2004).”
Constraints on Dark Matter Microphysics from the Milky Way Satellite Population (2019, background): “…dark matter (CDM) paradigm, structure forms from initial conditions described by a featureless power spectrum of matter perturbations, giving rise to a present-day dark matter (DM) halo mass function that extends uninterrupted down to sub-solar masses (Green et al. 2004; Diemand et al. 2005).”
Hidden charged dark matter (2009, methodology): “For a typical WIMP with electroweak scale mass, the kinetic decoupling temperature ranges roughly from 10 MeV to 1 GeV, which leads to the formation of dark matter halos with masses as small as 10M⊙ to 10M⊙ [29–31, 51–55].”