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Title:
Cold Dark Matter Substructure and Galactic Disks
Authors:
Kazantzidis, Stelios; Zentner, Andrew R.; Bullock, James S.
Affiliation:
AA(Center for Cosmology and Astro-Particle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USA ), AB(Department of Physics & Astronomy, University of Pittsburgh, 100 Allen Hall, 3941 O'Hara Street, Pittsburgh, PA 15260, USA ), AC(Center for Cosmology, Department of Physics & Astronomy, The University of California at Irvine, 4168 Reines Hall, Irvine, CA 92697, USA )
Publication:
The Galaxy Disk in Cosmological Context, Proceedings of the International Astronomical Union, IAU Symposium, Volume 254. Edited by J. Andersen, J. Bland-Hawthorn, and B. Nordström, p. 417-422
Publication Date:
03/2009
Origin:
CUP
Keywords:
cosmology: theory, dark matter, galaxies: formation, galaxies: dynamics, galaxies: structure, methods: numerical
DOI:
10.1017/S1743921308027907
Bibliographic Code:
2009IAUS..254..417K

Abstract

We perform a set of high-resolution, fully self-consistent dissipationless N-body simulations to investigate the influence of cold dark matter (CDM) substructure on the dynamical evolution of thin galactic disks. Our method combines cosmological simulations of galaxy-sized CDM halos to derive the properties of substructure populations and controlled numerical experiments of consecutive subhalo impacts onto initially-thin, fully-formed disk galaxies. We demonstrate that close encounters between massive subhalos and galactic disks since z ~ 1 should be common occurrences in ΛCDM models. In contrast, extremely few satellites in present-day CDM halos are likely to have a significant impact on the disk structure. One typical host halo merger history is used to seed controlled N-body experiments of subhalo-disk encounters. As a result of these accretion events, the disk thickens considerably at all radii with the disk scale height increasing in excess of a factor of 2 in the solar neighborhood. We show that interactions with the subhalo population produce a wealth of distinctive morphological signatures in the disk stars, many of which resemble those being discovered in the Milky Way (MW), M31, and in other disk galaxies, including: conspicuous flares; bars; low-lived, ring-like features in the outskirts; and low-density, filamentary structures above the disk plane. These findings highlight the significant role of CDM substructure in setting the structure of disk galaxies and driving galaxy evolution.
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