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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 709971.0, MPI für Astronomie / Publikationen_mpia
MaGICC baryon cycle: the enrichment history of simulated disc galaxies
Authors:Brook, C. B.; Stinson, G.; Gibson, B. K.; Shen, S.; Macciò, A. V.; Obreja, A.; Wadsley, J.; Quinn, T.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:Monthly Notices of the Royal Astronomical Society
Volume:443
Start Page:3809
End Page:3818
Audience:Not Specified
Abstract / Description:Using cosmological galaxy formation simulations from the MaGICC (Making Galaxies in a Cosmological Context) project, spanning stellar mass from ˜107 to 3 × 1010 M&sun;, we trace the baryonic cycle of infalling gas from the virial radius through to its eventual participation in the star formation process. An emphasis is placed upon the temporal history of chemical enrichment during its passage through the corona and circumgalactic medium. We derive the distributions of time between gas crossing the virial radius and being accreted to the star-forming region (which allows for mixing within the corona), as well as the time between gas being accreted to the star-forming region and then ultimately forming stars (which allows for mixing within the disc). Significant numbers of stars are formed from gas that cycles back through the hot halo after first accreting to the star-forming region. Gas entering high-mass galaxies is pre-enriched in low-mass proto-galaxies prior to entering the virial radius of the central progenitor, with only small amounts of primordial gas accreted, even at high redshift (z ˜ 5). After entering the virial radius, significant further enrichment occurs prior to the accretion of the gas to the star-forming region, with gas that is feeding the star-forming region surpassing 0.1 Z&sun; by z = 0. Mixing with halo gas, itself enriched via galactic fountains, is thus crucial in determining the metallicity at which gas is accreted to the disc. The lowest mass simulated galaxy (Mvir ˜ 2 × 1010 M&sun;, with M* ˜ 107 M&sun;), by contrast, accretes primordial gas through the virial radius and on to the disc, throughout its history. Much like the case for classical analytical solutions to the so-called `G-dwarf problem', overproduction of low-metallicity stars is ameliorated by the interplay between the time of accretion on to the disc and the subsequent involvement in star formation - i.e. due to the inefficiency of star formation. Finally, gas outflow/metal removal rates from star-forming regions as a function of galactic mass are presented.
Free Keywords:galaxies: evolution; galaxies: formation; galaxies: spiral
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0035-8711 %R 10.1093/mnras/stu1406
URL:http://adsabs.harvard.edu/abs/2014MNRAS.443.3809B
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