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Structure of dark matter haloes of Milky Way satellite galaxies in SIDM universes

Published online by Cambridge University Press:  30 October 2019

Takashi Okamoto Open the ORCID record for Takashi Okamoto [Opens in a new window]
Takashi Okamoto*
Affiliation:
Faculty of Science, Hokkaido Uniersity, N10 W8 Kitaku, Sapporo 060-0810 Japan email: okamoto@astro1.sci.hokudai.ac.jp
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Abstract

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Self-interacting dark matter (SIDM) can create sufficiently large cores in dark matter haloes of dwarf galaxies if the self-interaction cross-section is sufficiently large on scales of dwarf galaxies. Such a large cross-section can be realized without changing the densities and shapes of cluster-size haloes by introducing a velocity dependent cross-section. Lowering the central densities of dwarf-size haloes, however, may change the strength of stellar feedback required to reproduce observed properties of dwarf galaxies such as the luminosity function of the Milky Way’s satellite galaxies. We perform simulations of galaxy formation by employing such a velocity dependent self-interaction cross-section to investigate the coupled effect of SIDM and feedback.

Keywords

galaxies: dwarfgalaxies: formationcosmology: dark matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S344: Dwarf Galaxies: From the Deep Universe to the Present , August 2018 , pp. 498 - 501
Copyright
© International Astronomical Union 2019 

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