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Baryons and Dark Matter halo distributions in ΛCDM Cosmology

Published online by Cambridge University Press:  13 April 2010

Susana Pedrosa ,
Patricia Tissera  and
Cecilia Scannapieco
Susana Pedrosa
Affiliation:
Instituto de Astronomía y Física del Espacio, CONICET - UBA, CC67 Suc28, Ciudad Autónoma de Buenos Aires(1428), Argentina, email: supe@iafe.uba.ar Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina
Patricia Tissera
Affiliation:
Instituto de Astronomía y Física del Espacio, CONICET - UBA, CC67 Suc28, Ciudad Autónoma de Buenos Aires(1428), Argentina, email: supe@iafe.uba.ar Consejo Nacional de Investigaciones Científicas y Técnicas, Buenos Aires, Argentina
Cecilia Scannapieco
Affiliation:
Max Planck Institute for Astrophysics, Karl-Schwarzchild Str. 1, D85748, Garching, Germany
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Abstract

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We analyse the dark matter (DM) distribution in a ≈1012M⊙ halo 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.

Keywords

galaxies: halosgalaxies: structurecosmology: dark matter
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S262: Stellar Populations – Planning for the Next Decade , August 2009 , pp. 404 - 405
Copyright
Copyright © International Astronomical Union 2010

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