Stellar Halo Constraints on Simulated Late Type Galaxies

Abstract

How do late type spiral galaxies form within the context of a CDM cosmology? We contrast N-body, smoothed particle hydrodynamical simulations of galaxy formation which employ two different supernova feedback mechanisms. Observed mass and metallicity distributions of the stellar halos of the Milky Way and M31 provide constraints on these models. A strong feedback model, incorporating an adiabatic phase in star burst regions, better reproduces these observational properties than our comparative thermal feedback model. This demonstrates the importance of energy feedback in regulating star formation in small systems, which collapse at early epochs, in the evolution of late type disk galaxies.

arXiv comment5 pages, 5 figures, accepted for publication in MNRAS

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Cited by in corpus (61)

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• Galactic stellar haloes in the CDM model
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• The birth of the Milky Way as uncovered by accurate stellar ages with Gaia
• Lambda-Cold Dark Matter, Stellar Feedback, and the Galactic Halo Abundance Pattern
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• The role of mergers and halo spin in shaping galaxy morphology
• Implementation of feedback in SPH: towards concordance of methods
• The Metal-Poor Halo of the Andromeda Spiral Galaxy (M31)
• Vertical disc heating in Milky Way-sized galaxies in a cosmological context
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• Simulating the Mass-Metallicity Relation from z=1
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• The elusive stellar halo of the Triangulum Galaxy
• Heating and enriching the intracluster medium
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• Cosmological simulations of the high-redshift radio universe
• Gas Rich Mergers in Disk Formation
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