Inner structure of dark matter halos at high $z$ in cosmological models with non-power-law primordial spectra

Abstract

We consider three cosmological models with non-power-law spectra of primordial density perturbations and test them against $\Lambda$CDM in density profiles of dark matter halos. We found that, despite the significant difference in initial conditions, the mean density profiles of all models are still close to the Navarro-Frenk-White one, albeit with some dispersion. We demonstrate that the density profile slopes in the innermost part of halo have a significant evolution with $z$, which can be used to identify the cosmological model. We also present a toy model resulting in the appearance of core in the central part of dark matter halo.

11 pages, 6 figures, published in Phys. Rev. D (24 October 2024)

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Cited by in corpus (4)

• The Effects of Linear Matter Power Spectrum Enhancement on Dark Matter Substructure
• Cascade Relaxation of the Gravitating Vacuum as a Generator of the Evolving Universe
• Dark Secrets of Baryons: Illuminating Dark Matter-Baryon Interactions with JWST
• Absorption in the 21 cm Hydrogen Line at $z>10$ as a Sensitive Tool for the Construction of a Cosmological Model on Small Scales