Dark matter response to galaxy formation

We have resimulated the six galaxy-sized haloes of the Aquarius Project including metal-dependent cooling, star formation and supernova feedback. This allows us to study not only how dark matter haloes respond to galaxy formation, but also how this response is affected by details of halo assembly hi...

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Detalles Bibliográficos
Autores principales:	Tissera, P.B., White, S.D.M., Pedrosa, S., Scannapieco, C.
Formato:	JOUR
Materias:	Galaxies: evolution Galaxies: formation Galaxies: haloes
Acceso en línea:	http://hdl.handle.net/20.500.12110/paper_00358711_v406_n2_p922_Tissera
Aporte de:	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires

id	todo:paper_00358711_v406_n2_p922_Tissera
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spelling	todo:paper_00358711_v406_n2_p922_Tissera2023-10-03T14:46:58Z Dark matter response to galaxy formation Tissera, P.B. White, S.D.M. Pedrosa, S. Scannapieco, C. Galaxies: evolution Galaxies: formation Galaxies: haloes We have resimulated the six galaxy-sized haloes of the Aquarius Project including metal-dependent cooling, star formation and supernova feedback. This allows us to study not only how dark matter haloes respond to galaxy formation, but also how this response is affected by details of halo assembly history. In agreement with previous work, we find baryon condensation to lead to increased dark matter concentration. Dark matter density profiles differ substantially in shape from halo to halo when baryons are included, but in all cases the velocity dispersion decreases monotonically with radius. Some haloes show an approximately constant dark matter velocity anisotropy with β ≈ 0.1-0.2, while others retain the anisotropy structure of their baryon-free versions. Most of our haloes become approximately oblate in their inner regions, although a few retain the shape of their dissipationless counterparts. Pseudo-phase-space densities are described by a power law in radius of altered slope when baryons are included. The shape and concentration of the dark matter density profiles are not well reproduced by published adiabatic contraction models. The significant spread we find in the density and kinematic structure of our haloes appears related to differences in their formation histories. Such differences already affect the final structure in baryon-free simulations, but they are reinforced by the inclusion of baryons, and new features are produced. The details of galaxy formation need to be better understood before the inner dark matter structure of galaxies can be used to constrain cosmological models or the nature of dark matter. © 2010 The Authors. Journal compilation © 2010 RAS. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00358711_v406_n2_p922_Tissera
institution	Universidad de Buenos Aires
institution_str	I-28
repository_str	R-134
collection	Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic	Galaxies: evolution Galaxies: formation Galaxies: haloes
spellingShingle	Galaxies: evolution Galaxies: formation Galaxies: haloes Tissera, P.B. White, S.D.M. Pedrosa, S. Scannapieco, C. Dark matter response to galaxy formation
topic_facet	Galaxies: evolution Galaxies: formation Galaxies: haloes
description	We have resimulated the six galaxy-sized haloes of the Aquarius Project including metal-dependent cooling, star formation and supernova feedback. This allows us to study not only how dark matter haloes respond to galaxy formation, but also how this response is affected by details of halo assembly history. In agreement with previous work, we find baryon condensation to lead to increased dark matter concentration. Dark matter density profiles differ substantially in shape from halo to halo when baryons are included, but in all cases the velocity dispersion decreases monotonically with radius. Some haloes show an approximately constant dark matter velocity anisotropy with β ≈ 0.1-0.2, while others retain the anisotropy structure of their baryon-free versions. Most of our haloes become approximately oblate in their inner regions, although a few retain the shape of their dissipationless counterparts. Pseudo-phase-space densities are described by a power law in radius of altered slope when baryons are included. The shape and concentration of the dark matter density profiles are not well reproduced by published adiabatic contraction models. The significant spread we find in the density and kinematic structure of our haloes appears related to differences in their formation histories. Such differences already affect the final structure in baryon-free simulations, but they are reinforced by the inclusion of baryons, and new features are produced. The details of galaxy formation need to be better understood before the inner dark matter structure of galaxies can be used to constrain cosmological models or the nature of dark matter. © 2010 The Authors. Journal compilation © 2010 RAS.
format	JOUR
author	Tissera, P.B. White, S.D.M. Pedrosa, S. Scannapieco, C.
author_facet	Tissera, P.B. White, S.D.M. Pedrosa, S. Scannapieco, C.
author_sort	Tissera, P.B.
title	Dark matter response to galaxy formation
title_short	Dark matter response to galaxy formation
title_full	Dark matter response to galaxy formation
title_fullStr	Dark matter response to galaxy formation
title_full_unstemmed	Dark matter response to galaxy formation
title_sort	dark matter response to galaxy formation
url	http://hdl.handle.net/20.500.12110/paper_00358711_v406_n2_p922_Tissera
work_keys_str_mv	AT tisserapb darkmatterresponsetogalaxyformation AT whitesdm darkmatterresponsetogalaxyformation AT pedrosas darkmatterresponsetogalaxyformation AT scannapiecoc darkmatterresponsetogalaxyformation
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Dark matter response to galaxy formation

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