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The inner structure of dark matter haloes in the Hubble sequence

Antonino Del Popolo

Dipartimento di Fisica e Astronomia, University of Catania, Viale Andrea Doria 6, 95125 Catania, Italy

INFN Sezione di Catania, Via S. Sofia 64, I-95123 Catania, Italy

International Institute of Physics, Universidade Federal do Rio Grande do Norte, 59012-970 Natal, Brazil

E-mail Address: adelpopolo@oact.inaf.it

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Anna Saburova

Sternberg Astronomical Institute, Moscow M.V. Lomonosov State University, Russia

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, and

Gaetano Belvedere

Dipartimento di Fisica e Astronomia, Università di Catania, Sezione Astrofisica, Via Santa Sofia 78, I-95125, Catania, Italy

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https://doi.org/10.1142/S0218271816500930Cited by:0 (Source: Crossref)

Abstract

We study how galaxy morphology changes the relation among the inner slope $α$ of galactic density profiles and the stellar mass, and rotation velocity.

We find that the slope $α$ flattens monotonically from $α ≃ - 1$ to $α ≃ 0$ going from giant galaxies (ellipticals, spirals) to dwarf galaxies ( $≃ 1 0^{8} M_{*}$ ). At masses smaller than $≃ 1 0^{8} M_{*}$ , in the mass range dominated by nonrotational supported galaxies (e.g. dSphs), the slope steepens due to the offset in angular momentum of rotational dominated, and nonrotational dominated galaxies.

A comparison with SPH simulations finds our result in qualitative agreement with them, but the inner slope $α$ at small stellar masses is flatter than that in their simulations. Density profiles become cuspy for $M_{*}$ in the range $1 0^{4}$ – $1 0^{5} M_{⊙}$ , similarly to Õnorbe.

Keywords:

PACS: 95.35+d, 95.30.Cq, 97.20.Vs, 98.35.Gi, 98.80.Cq

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