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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 720206.0, MPI für Astronomie / Publikationen_mpia
How to bend galaxy disc profiles: the role of halo spin
Authors:Herpich, J.; Stinson, G. S.; Dutton, A. A.; Rix, H. -. W.; Martig, M.; Roškar, R.; Macciò, A. V.; Quinn, T. R.; Wadsley, J.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:Monthly Notices of the Royal Astronomical Society
Start Page:L99
End Page:L103
Audience:Not Specified
Abstract / Description:The radial density profiles of stellar galaxy discs can be well approximated as an exponential. Compared to this canonical form, however, the profiles in the majority of disc galaxies show downward or upward breaks at large radii. Currently, there is no coherent explanation in a galaxy formation context of the radial profile per se, along with the two types of profile breaks. Using a set of controlled hydrodynamic simulations of disc galaxy formation, we find a correlation between the host halo's initial angular momentum and the resulting radial profile of the stellar disc: galaxies that live in haloes with a low spin parameter λ ≲ 0.03 show an up-bending break in their disc density profiles, while galaxies in haloes of higher angular momentum show a down-bending break. We find that the case of pure exponential profiles (λ ≈ 0.035) coincides with the peak of the spin parameter distribution from cosmological simulations. Our simulations not only imply an explanation of the observed behaviours, but also suggest that the physical origin of this effect is related to the amount of radial redistribution of stellar mass, which is anticorrelated with λ.
Free Keywords:hydrodynamics; methods: numerical; galaxies: spiral; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnrasl/slv006
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