Abstract
We use a semi-analytic model of halo formation to study the dynamical history of giant field galaxies like the Milky Way. We find that in a concordance LCDM cosmology, most isolated disk galaxies have remained undisturbed for 8–10 Gyr, such that the age of the Milky Way’s thin disk is unremarkable. Many systems also have older disk components which have been thickened by minor mergers, consistent with recent observations of nearby field galaxies. We do have a considerable problem, however, reproducing the morphological mix of nearby galaxies. In our fiducial model, most systems have disk-to-bulge mass ratios of order 1, and look like SOs rather than spirals. This result depends mainly on merger statistics, and is unchanged for most reasonable choices of our model parameters. We discuss two possible solutions to this morphology problem in LCDM.
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© 2003 Springer Science+Business Media Dordrecht
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Taylor, J.E., Babul, A. (2003). Modelling the Formation of Individual Galaxies: A Morphology Problem for CDM?. In: Hensler, G., Stasińska, G., Harfst, S., Kroupa, P., Theis, C. (eds) The Evolution of Galaxies. Springer, Dordrecht. https://doi.org/10.1007/978-94-017-3315-1_20
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DOI: https://doi.org/10.1007/978-94-017-3315-1_20
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-481-6248-2
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