Dark matter response to galaxy formation

By Patricia B. Tissera, Simon D. M. White, S. Pedrosa, Cecilia Scannapieco Consejo Nacional de Investigaciones Ci Tecnicas, Conicet, A. I. D. A. Y. F. D. Espacio, A. L. M. F. Astrophysics, G. Potsdam, Heidelberg · Germany. 2009

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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.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/20be56ac600e5d342732dfc8c753ae0d8036a3ed

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Citations in the corpus

Co-formation of the disc and the stellar halo (2018, background): “On the other hand, when the Aquarius halos are re-simulated with added gas physics and star-formation, only some galaxies retain their DM-only anisotropy trends, while in others, the β profile flattens and stays constant with β ∼ 0.2 throughout the galaxy (see Tissera et al. 2010).”
Two-dimensional kinematics of SLACS lenses – III. Mass structure and dynamics of early-type lens galaxies beyond z ≃ 0.1 (2011, background): “The high-resolution simulations of moderately massive ystems (with halo masses comparable to that of the Milky Way) carried out by Tissera et al. (2010), which include a detailed tratment of baryonic processes, reveal a nearly isothermal profile over a relatively large radial range extending up to…”
The shape of dark matter haloes in the Aquarius simulations: evolution and memory (2011, background): “However, the work of Tissera et al. (2010); Abadi et al. (2010); Bett et al. (2010) shows that even though the halo axis ratios c© 2011 RAS, MNRAS 000, 1–11 increase when a disc is formed (i.e. they become rounder), the trends with radius appear to be preserved.”
Chemical signatures of formation processes in the stellar populations of simulated galaxies (2011, background): “Scannapieco et al. (2009, 2011) and Tissera et al. (2010) who reported good agreement between their dynamical and structural properties and those of Aq-E-5, 2 Simulations Aq-E-6 and Aq-E-7 correspond to those labeled as Aq-E-6b and Aq-E-6 in Scannapieco et al. (2011) c© 0000 RAS, MNRAS 000,…”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, background): “More recent simulations indicate an even smaller compression (Tissera et al. 2010; Duffy et al. 2010).”
Erratum: From dwarf spheroidals to cD galaxies: simulating the galaxy population in a ΛCDM cosmology (2010, background): “…adopted by Cole et al. (2000) appears to overestimate the effect of baryons, and at least some recent simulations suggest that the maximum halo circular velocity found in an equivalent dark matter only simulation may be a good approximation to the disk rotation velocity (e.g. Tissera et al. 2010).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “Recent hydrodynamical simulations of galaxy formation yield even weaker halo contraction (Abadi et al. 2010; Duffy et al. 2010; Pedrosa et al. 2010; Tissera et al. 2010).”
The kinematic connection between galaxies and dark matter haloes (2010, background): “The magenta diamonds show the simulations of Tissera et al. (2009), where we have estimated Vopt from their Figure 9.”