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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 693448.0, MPI für Astronomie / Publikationen_mpia
MaGICC thick disc - I. Comparing a simulated disc formed with stellar feedback to the Milky Way
Authors:Stinson, G. S.; Bovy, J.; Rix, H. -. W.; Brook, C.; Roškar, R.; Dalcanton, J. J.; Macciò, A. V.; Wadsley, J.; Couchman, H. M. P.; Quinn, T. R.
Date of Publication (YYYY-MM-DD):2013
Title of Journal:Monthly Notices of the Royal Astronomical Society
Issue / Number:1
Start Page:625
End Page:634
Audience:Not Specified
Abstract / Description:We analyse the structure and chemical enrichment of a Milky Way-like galaxy with a stellar mass of 2 × 1010 M, formed in a cosmological hydrodynamical simulation. It is disc dominated with a flat rotation curve, and has a disc scalelength similar to the Milky Way's, but a velocity dispersion that is ˜50 per cent higher. Examining stars in narrow [Fe/H] and [α/Fe] abundance ranges, we find remarkable qualitative agreement between this simulation and observations. (a) The old stars lie in a thickened distribution with a short scalelength, while the young stars form a thinner disc, with scalelengths decreasing, as [Fe/H] increases. (b) Consequently, there is a distinct outward metallicity gradient. (c) Mono-abundance populations exist with a continuous distribution of scaleheights (from thin to thick). However, the simulated galaxy has a distinct and substantive very thick disc (hz ˜ 1.5 kpc), not seen in the Milky Way. The broad agreement between simulations and observations allows us to test the validity of observational proxies used in the literature: we find in the simulation that mono-abundance populations are good proxies for single age populations (<1 Gyr) for most abundances.
Free Keywords:hydrodynamics; galaxies: formation; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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