High-resolution simulations of the reionization of an isolated milky way-M31 galaxy pair
Entity
UAM. Departamento de Física TeóricaPublisher
The American Astronomical SocietyDate
2013-10-15Citation
10.1088/0004-637X/777/1/51
The Astrophysical Journal 777.1 (2013): 51
ISSN
0004-637X (print); 1538-4357 (online)DOI
10.1088/0004-637X/777/1/51Funded by
A.K. is supported by the Spanish Ministerio de Ciencia e Innovación (MICINN) in Spain through the Ramón y Cajal program as well as the grants CSD2009-00064 and CAM S2009/ESP-1496 and the Ministerio de Economía y Competitividad (MINECO) through grant AYA2012-31101. He further thanks Peter Thomas for angels who burn their wings. G.Y. acknowledges support from MICINN under research grants AYA2009-13875-C03-02, FPA2009-08958Project
Comunidad de Madrid. S2009/ESP-1496/ASTROMADRIDEditor's Version
http://dx.doi.org/10.1088/0004-637X/777/1/51Subjects
Cosmology: theory; Galaxies: formation; Galaxies: high-redshift; Methods: numerical; Radiative transfer; Intergalactic medium; FísicaNote
The Astrophysical Journal 777.1 (2013): 51 reproduced by permission of the AASRights
© 2013. The American Astronomical SocietyAbstract
We present the results of a set of numerical simulations aimed at studying reionization at the galactic scale. We use a high-resolution realization of the formation of the Milky Way (MW)-M31 system to simulate the reionization of the Local Group. The reionization calculation was performed with the post-processing radiative transfer code ATON and the underlying cosmological simulation was performed as part of the CLUES project (http://www.clues-project.org). We vary the source models to bracket the range of source properties used in the literature. We investigate the structure and propagation of the galactic ionization fronts by a visual examination of our reionization maps. Within the progenitors, we find that reionization is patchy and proceeds locally inside-out. The process becomes patchier with decreasing source photon output. It is generally dominated by one major H II region and one to four additional isolated smaller bubbles, which eventually overlap. Higher emissivity results in faster and earlier local reionization. In all models, the reionization of the MW and M31 are similar in duration, i.e., between 203 Myr and 22 Myr depending on the source model, placing their z reion between 8.4 and 13.7. In all models except the most extreme, the MW and M31 progenitors reionize internally, ignoring each other despite being relatively close to each other, even during the epoch of reionization. Only in the case of strong supernova feedback suppressing star formation in halos less massive than 109 M ⊙, and using our highest emissivity, do we find that the MW is reionized by M31
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Google Scholar:Ocvirk, Pierre
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Aubert, Dominique
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Chardin, Jonathan
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Knebe, Alexander
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Gottlöber, Stefan
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Yepes Alonso, Gustavo
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Hoffman, Yehuda
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Libeskind, Noam I.
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