Volume 622, February 2019
|Number of page(s)||17|
|Published online||19 February 2019|
Dark matter response to galaxy assembly history
Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstrasse 25/8, 6020 Innsbruck, Austria
e-mail: Maria.Artale@uibk.ac.at; firstname.lastname@example.org
2 CONICET-Universidad de Buenos Aires, Instituto de Astronomía y Física del Espacio (IAFE), CC 67, Suc. 28, 1428 Buenos Aires, Argentina
3 Departamento de Ciencias Físicas, Universidad Andres Bello, Av. Republica 220, Santiago, Chile
4 Instituto de Física de Buenos Aires, IFIBA, UBA CONICET, Pabellon 1, Ciudad Universitaria, 1428 Buenos Aires, Argentina
5 Instituto de Astrofísica de Canarias, Calle Via Láctea, La Laguna, Tenerife, Spain
6 University of La Laguna, Avda. Astrofísico Fco. Sánchez, La Laguna, Tenerife, Spain
Accepted: 7 January 2019
Aims. It is well known that the presence of baryons affects the dark matter host haloes. Exploring the galaxy assembly history together with the dark matter haloes properties through time can provide a way to measure these effects.
Methods. We have studied the properties of four Milky Way mass dark matter haloes from the Aquarius project during their assembly history, between z = 0 − 4. In this work, we used a published SPH run and the dark matter only counterpart as case studies. To asses the robustness of our findings, we compared them with one of the haloes run using a moving-mesh technique and different sub-grid scheme.
Results. Our results show that the cosmic evolution of the dark matter halo profiles depends on the assembly history of the baryons. We find that the dark matter profiles do not significantly change with time, hence they become stable, when the fraction of baryons accumulated in the central regions reaches 80 per cent of its present mass within the virial radius. Furthermore, the mass accretion history shows that the haloes that assembled earlier are those that contain a larger amount of baryonic mass aforetime, which in turn allows the dark matter halo profiles to reach a stable configuration earlier. For the SPH haloes, we find that the specific angular momentum of the dark matter particles within the five per cent of the virial radius at z = 0, remains approximately constant from the time at which 60 per cent of the stellar mass is gathered. We have explored different theoretical and empirical models for the contraction of the haloes through redshift. A model to better describe the contraction of the haloes through redshift evolution must depend on the stellar mass content in the inner regions.
Key words: galaxies: halos / Galaxy: evolution / Galaxy: formation
© ESO 2019
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