Baryons and dark matter halo distributions in ACDM cosmology

Susana Pedrosa, Patricia Tissera, Cecilia Scannapieco

Resultado de la investigación: Article

Resumen

We analyse the dark matter (DM) distribution in a ≈ 10 M alo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy. The accretion of satellites could be associated with an expansion of the dark matter profiles, triggered by angular momentum transfer from the incoming satellites. However, we also found that these mechanism have different efficiencies which are set by the history of formation of the structure.

Idioma originalEnglish
Páginas (desde-hasta)404-405
Número de páginas2
PublicaciónProceedings of the International Astronomical Union
Volumen5
N.ºS262
DOI
EstadoPublished - 1 ago 2009

Huella dactilar

cosmology
baryons
halos
dark matter
profiles
histories
galaxies
momentum transfer
history
angular momentum
physics
assembly
accretion
distribution
stars
expansion
gases
gas
simulation

ASJC Scopus subject areas

  • Astronomy and Astrophysics

Citar esto

Pedrosa, Susana ; Tissera, Patricia ; Scannapieco, Cecilia. / Baryons and dark matter halo distributions in ACDM cosmology. En: Proceedings of the International Astronomical Union. 2009 ; Vol. 5, N.º S262. pp. 404-405.
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Baryons and dark matter halo distributions in ACDM cosmology. / Pedrosa, Susana; Tissera, Patricia; Scannapieco, Cecilia.

En: Proceedings of the International Astronomical Union, Vol. 5, N.º S262, 01.08.2009, p. 404-405.

Resultado de la investigación: Article

TY - JOUR

T1 - Baryons and dark matter halo distributions in ACDM cosmology

AU - Pedrosa, Susana

AU - Tissera, Patricia

AU - Scannapieco, Cecilia

PY - 2009/8/1

Y1 - 2009/8/1

N2 - We analyse the dark matter (DM) distribution in a ≈ 10 M ⊙alo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy. The accretion of satellites could be associated with an expansion of the dark matter profiles, triggered by angular momentum transfer from the incoming satellites. However, we also found that these mechanism have different efficiencies which are set by the history of formation of the structure.

AB - We analyse the dark matter (DM) distribution in a ≈ 10 M ⊙alo extracted from a simulation consistent with the concordance cosmology, where the physics regulating the transformation of gas into stars was allowed to change producing galaxies with different morphologies. Although the DM profiles get more concentrated as baryons are collected at the centre of the haloes compared to a pure dynamical run, the total baryonic mass alone is not enough to fully predict the reaction of the DM profile. Our findings suggest that the response of the DM halo is driven by the history of assembly of baryons into a galaxy. The accretion of satellites could be associated with an expansion of the dark matter profiles, triggered by angular momentum transfer from the incoming satellites. However, we also found that these mechanism have different efficiencies which are set by the history of formation of the structure.

KW - Cosmology: dark matter

KW - Galaxies: halos

KW - Galaxies: structure

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