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Baryonic and dark matter distribution in cosmological simulations of spiral galaxies


Mollitor, Pol; Nezri, Emmanuel; Teyssier, Romain (2015). Baryonic and dark matter distribution in cosmological simulations of spiral galaxies. Monthly Notices of the Royal Astronomical Society, 447(2):1353-1369.

Abstract

We study three cosmological hydrodynamical simulations of Milky Way(MW)-sized haloes including a comparison with the dark matter(DM)-only counterparts. We find one of our simulated galaxies with interesting MW-like features. Thanks to a consistently tuned star formation rate and supernovae feedback we obtain an extended disc and a flat rotation curve with a satisfying circular velocity and a reasonable DM density in the solar neighbourhood. Mimicking observational methods, we re-derive the stellar mass and obtain stellar-to-halo mass ratios reduced by more than 50 per cent. We show the interaction between the baryons and the DM which is first contracted by star formation and then cored by feedback processes. Indeed, we report an unprecedentedly observed effect in the DM density profile consisting of a central core combined with an adiabatic contraction at larger galactic radii. The cores obtained are typically ˜5 kpc large. Moreover, this also impacts the DM density at the solar radius. In our simulation resembling most to the MW, the density is raised from 0.23 GeV $cm^3$ in the DM only run to 0.36 GeV $cm^3$ (spherical shell) or 0.54 GeV $cm^3$ (circular ring) in the hydrodynamical run. Studying the subhaloes, the DM within luminous satellites is also affected by baryonic processes and exhibits cored profiles whereas dark satellites are cuspy. We find a shift in mass compared to DM-only simulations and obtain, for haloes in the lower MW mass range, a distribution of luminous satellites comparable to the MW spheroidal dwarf galaxies.

Abstract

We study three cosmological hydrodynamical simulations of Milky Way(MW)-sized haloes including a comparison with the dark matter(DM)-only counterparts. We find one of our simulated galaxies with interesting MW-like features. Thanks to a consistently tuned star formation rate and supernovae feedback we obtain an extended disc and a flat rotation curve with a satisfying circular velocity and a reasonable DM density in the solar neighbourhood. Mimicking observational methods, we re-derive the stellar mass and obtain stellar-to-halo mass ratios reduced by more than 50 per cent. We show the interaction between the baryons and the DM which is first contracted by star formation and then cored by feedback processes. Indeed, we report an unprecedentedly observed effect in the DM density profile consisting of a central core combined with an adiabatic contraction at larger galactic radii. The cores obtained are typically ˜5 kpc large. Moreover, this also impacts the DM density at the solar radius. In our simulation resembling most to the MW, the density is raised from 0.23 GeV $cm^3$ in the DM only run to 0.36 GeV $cm^3$ (spherical shell) or 0.54 GeV $cm^3$ (circular ring) in the hydrodynamical run. Studying the subhaloes, the DM within luminous satellites is also affected by baryonic processes and exhibits cored profiles whereas dark satellites are cuspy. We find a shift in mass compared to DM-only simulations and obtain, for haloes in the lower MW mass range, a distribution of luminous satellites comparable to the MW spheroidal dwarf galaxies.

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Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Language:English
Date:February 2015
Deposited On:22 Feb 2016 14:24
Last Modified:05 Apr 2016 20:05
Publisher:Oxford University Press
ISSN:0035-8711
Additional Information:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2015 The Authors Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.
Free access at:Publisher DOI. An embargo period may apply.
Publisher DOI:https://doi.org/10.1093/mnras/stu2466
Other Identification Number:arXiv:1405.4318v2

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