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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 606578.0, MPI für Astronomie / Publikationen_mpia
The effects of a hot gaseous halo in galaxy major mergers
Authors:Moster, B. P.; Macciò, A. V.; Somerville, R. S.; Naab, T.; Cox, T. J.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:Monthly Notices of the Royal Astronomical Society
Volume:415
Start Page:3750
End Page:3770
Audience:Not Specified
Abstract / Description:Cosmological hydrodynamical simulations as well as observations indicate that spiral galaxies comprise five different components: dark matter halo, stellar disc, stellar bulge, gaseous disc and gaseous halo. While the first four components have been extensively considered in numerical simulations of binary galaxy mergers, the effect of a hot gaseous halo has usually been neglected even though it can contain up to 80 per cent of the total gas within the galaxy virial radius. We present a series of hydrodynamic simulations of major mergers of disc galaxies, that for the first time include a diffuse, rotating, hot gaseous halo. Through cooling and accretion, the hot halo can dissipate and refuel the cold gas disc before and after a merger. This cold gas can subsequently form stars, thus impacting the morphology and kinematics of the remnant. Simulations of isolated systems with total mass MËœ 1012 M&sun; show a nearly constant star formation rate of Ëœ5 M&sun; yr-1 if the hot gaseous halo is included, while the star formation rate declines exponentially if it is neglected. We conduct a detailed study of the star formation efficiency during mergers and find that the presence of a hot gaseous halo reduces the starburst efficiency (e= 0.5) compared to simulations without a hot halo (e= 0.68). The ratio of the peak star formation rate in mergers compared to isolated galaxies is reduced by almost an order of magnitude (from 30 to 5). Moreover, we find cases where the stellar mass of the merger remnant is lower than the sum of the stellar mass of the two progenitor galaxies when evolved in isolation. This suggests a revision to semi-analytic galaxy formation models which assume that a merger always leads to enhanced star formation. In addition, the bulge-to-total ratio after a major merger is decreased if hot gas is included in the halo, due to the formation of a more massive stellar disc in the remnant. We show that adding the hot gas component has a significant effect on the kinematics and internal structure of the merger remnants, like an increased abundance of fast rotators and an r1/4 surface brightness profile at small scales. The consequences on the population of elliptical galaxies formed by disc mergers are discussed.
Free Keywords:methods: numerical; galaxies: elliptical and lenticular; cD; galaxies: haloes; galaxies: interactions; galaxies: starburst; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://cdsads.u-strasbg.fr/abs/2011MNRAS.415.3750M
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