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http://hdl.handle.net/2445/65672
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DC Field | Value | Language |
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dc.contributor.author | Manrique Oliva, Alberto | - |
dc.contributor.author | Salvador Solé, Eduard | - |
dc.contributor.author | Juan Rovira, Enric | - |
dc.contributor.author | Hatziminaoglou, Evanthia | - |
dc.contributor.author | Rozas, José María | - |
dc.contributor.author | Sagristà, Antoni | - |
dc.contributor.author | Casteels, Kevin R. V | - |
dc.contributor.author | Bruzual, Gustavo | - |
dc.contributor.author | Magris, Gladis | - |
dc.date.accessioned | 2015-05-28T12:26:46Z | - |
dc.date.available | 2015-05-28T12:26:46Z | - |
dc.date.issued | 2015-01-06 | - |
dc.identifier.issn | 0067-0049 | - |
dc.identifier.uri | http://hdl.handle.net/2445/65672 | - |
dc.description.abstract | We present an Analytic Model of Intergalactic-medium and GAlaxy (AMIGA) evolution since the dark ages. AMIGA is in the spirit of the popular semi-analytic models of galaxy formation, although it does not use halo merger trees but interpolates halo properties in grids that are progressively built. This strategy is less memory-demanding and allows one to start modeling at sufficiently high redshifts and low halo masses to have trivial boundary conditions. The number of free parameters is minimized by making a causal connection between physical processes usually treated as independent of each other, which leads to more reliable predictions. However, the strongest points of AMIGA are the following: (1) the inclusion of molecular cooling and metal-poor, population III (Pop III) stars with the most dramatic feedback and (2) accurate follow up of the temperature and volume filling factor of neutral, singly ionized, and doubly ionized regions, taking into account the distinct halo mass functions in those environments. We find the following general results. Massive Pop III stars determine the intergalactic medium metallicity and temperature, and the growth of spheroids and disks is self-regulated by that of massive black holes (MBHs) developed from the remnants of those stars. However, the properties of normal galaxies and active galactic nuclei appear to be quite insensitive to Pop III star properties due to the much higher yield of ordinary stars compared to Pop III stars and the dramatic growth of MBHs when normal galaxies begin to develop, which cause the memory loss of the initial conditions. | - |
dc.format.extent | 17 p. | - |
dc.format.mimetype | application/pdf | - |
dc.language.iso | eng | - |
dc.publisher | Institute of Physics (IOP) | - |
dc.relation.isformatof | Reproducció del document publicat a: http://dx.doi.org/10.1088/0067-0049/216/1/13 | - |
dc.relation.ispartof | Astrophysical Journal Supplement Series, 2015, vol. 216, num. 1, p. 1-17 | - |
dc.relation.uri | http://dx.doi.org/10.1088/0067-0049/216/1/13 | - |
dc.rights | (c) American Astronomical Society, 2015 | - |
dc.source | Articles publicats en revistes (Física Quàntica i Astrofísica) | - |
dc.subject.classification | Matèria fosca (Astronomia) | - |
dc.subject.classification | Evolució de les galàxies | - |
dc.subject.classification | Galàxies | - |
dc.subject.classification | Formació de les galàxies | - |
dc.subject.other | Dark matter (Astronomy) | - |
dc.subject.other | Galaxies evolution | - |
dc.subject.other | Galaxies | - |
dc.subject.other | Galaxy formation | - |
dc.title | Leaving the Dark ages with AMIGA | - |
dc.type | info:eu-repo/semantics/article | - |
dc.type | info:eu-repo/semantics/publishedVersion | - |
dc.identifier.idgrec | 646087 | - |
dc.date.updated | 2015-05-28T12:26:52Z | - |
dc.rights.accessRights | info:eu-repo/semantics/openAccess | - |
Appears in Collections: | Articles publicats en revistes (Física Quàntica i Astrofísica) |
Files in This Item:
File | Description | Size | Format | |
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646087.pdf | 762.75 kB | Adobe PDF | View/Open |
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