Simulating Galaxies and Galaxy Clusters

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dc.creatorSommer-Larsen, Jesper
dc.date2004-04-01
dc.date.accessioned2026-07-07T02:12:48Z
dc.date.available2026-07-07T02:12:48Z
dc.descriptionThe X-ray luminosities of the hot halo gas around simulated, Milky Way like disk galaxies have been determined, as a function of redshift. The X-ray luminosity increases significantly with redshift, in some cases as much as a factor 30 going from z=0 to 2. Consequently, the optimal detection redshift can be >~0.5. Results of fully cosmological simulations of galaxy groups and clusters, incorporating star formation, chemical evolution with non-instantaneous recycling, metal-dependent radiative cooling, galactic super-winds and thermal conduction are presented. X-ray luminosities at z=0 are somewhat high and central entropies somewhat low compared to observations. This is likely a combined effect of chemical evolution and metal-dependent, radiative cooling. Central ICM abundance profiles are somewhat steep, and the observed level of ICM enrichment can only be reproduced with IMFs more top-heavy than the Salpeter IMF. In agreement with observations it is found that the iron in the ICM is in place already at z~1. The [Si/Fe] of the ICM decreases with time, and increases slightly with radius at a given time. The cluster galaxies match the observed "red sequence" very well, and the metallicity of cluster galaxies increases with galaxy mass, as observed.
dc.description6 pages, 2 B/W + 5 colour figures. Proceedings of the Vulcano conference on "Modelling the intergalactic and intracluster media", V. Antonuccio et al. (eds.), to be published online on MemSAIt - Supplementi. Printing in colour recommended
dc.identifierhttps://arxiv.org/abs/astro-ph/0404023
dc.identifierhttp://arxiv.org/abs/astro-ph/0404023
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/7581
dc.subjectAstrophysics
dc.titleSimulating Galaxies and Galaxy Clusters
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