MaGICC baryon cycle: the enrichment history of simulated disc galaxies

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dc.creator Brook, C. B.
dc.creator Stinson, G.
dc.creator Gibson, Brad K.
dc.creator Shen, S.
dc.creator Maccio, A. V.
dc.creator Obreja, A.
dc.creator Wadsley, J.
dc.creator Quinn, T.
dc.date.accessioned 2018-04-10T14:50:37Z
dc.date.available 2018-04-10T14:50:37Z
dc.date.issued 2014-10-01
dc.identifier.issn 0035-8711
dc.identifier.uri http://library2.smu.ca/handle/01/27399
dc.description Publisher's Version/PDF
dc.description.abstract Using cosmological galaxy formation simulations from the MaGICC (Making Galaxies in a Cosmological Context) project, spanning stellar mass from &sim;10<sup>7</sup> to 3 &times; 10<sup>10</sup> M<sub>☉</sub>, 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 starforming 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 &sim; 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<sub>☉</sub> 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 (M<sub>vir</sub> &sim; 2 &times; 10<sup>10</sup> M<sub>☉</sub>, with M<sub>★</sub> &sim; 10<sup>7</sup> M<sub>☉</sub>), 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 &lsquo;G-dwarf problem&rsquo;, 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 &ndash; 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.&nbsp; en_CA
dc.language.iso en en_CA
dc.publisher Oxford University Press en_CA
dc.relation.uri https://dx.doi.org/10.1093/mnras/stu1406
dc.rights This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.subject.lcsh Galaxies -- Evolution
dc.subject.lcsh Galaxies -- Formation
dc.subject.lcsh Simulation methods
dc.title MaGICC baryon cycle: the enrichment history of simulated disc galaxies en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Monthly Notices of the Royal Astronomical Society 443(4), 3809-3818. (2014) en_CA


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This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
 
Published Version: https://dx.doi.org/10.1093/mnras/stu1406
 
 

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