Formation of Milky Way-type stellar haloes in a Λ-CDM cosmology

Details Formation of Milky Way-type stellar haloes in a Λ-CDM cosmology Formation of Milky Way-type stellar haloes in a Λ-CDM cosmology

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012epjwc..1901002f&link_type=abstract

Assembling the Puzzle of the Milky Way, Le Grand-Bornand, France, Edited by C. Reylé; A. Robin; M. Schultheis; EPJ Web of Confer

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Scientific paper

Recent observations suggest that the Milky Way stellar halo has a `dual nature', meaning that both dissipational and dissipationless processes play a role in its build-up. The GIMIC suite of cosmological hydro-dynamical simulations show that, for Milky Way-mass haloes, in situ star formation is the dominant factor in the inner < 20 - 30 kpc, while tidal disruption of satellite galaxies contributes primarily to the outer regions. The in situ stars are found to originate in the earlier disc, at redshifts ~ 1- 1.5, and subsequently diffusing out of the disc by dynamical heating associated with mergers. The in situ component has a more flattened shape, a net prograde rotation and more metal-rich populations, in quantitative agreement with the observations. We conclude that the dual nature of the stellar halo is entirely compatible with the currently favoured Λ-CDM model.

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