On the evolution of the Fe abundance and of the Type Ia SN rate in clusters of galaxies

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dc.creatorCalura, Francesco
dc.creatorMatteucci, Francesca
dc.creatorTozzi, Paolo
dc.creator-
dc.date2007-02-27
dc.date.accessioned2026-07-07T10:36:54Z
dc.date.available2026-07-07T10:36:54Z
dc.descriptionThe study of the Fe abundance in the intra cluster medium (ICM) provides strong constraints on the integrated star formation history and supernova rate of the cluster galaxies, as well as on the ICM enrichment mechanisms. In this Letter, using chemical evolution models for galaxies of different morphological types, we study the evolution of the Fe content of clusters of galaxies. We assume that the ICM Fe enrichment occurs by means of galactic winds arising from elliptical galaxies and from gas stripped from the progenitors of S0 galaxies via external mechanisms, due to the interaction of the inter stellar medium with the ICM. The Fe-rich gas ejected by ellipticals accounts for the X_Fe,ICM values observed at z > 0.5, whereas the gas stripped from the progenitors of the S0 galaxies accounts for the increase of X_Fe,ICM observed at z<0.5. We tested two different scenarios for Type Ia supernova (SN) progenitors and we model the Type Ia SN rate observed in clusters, finding a good agreement between our predictions and the available observations.
dc.descriptionMNRAS, in press, 6 pages, 2 figures
dc.identifierhttps://arxiv.org/abs/astro-ph/0702714
dc.identifierhttp://arxiv.org/abs/astro-ph/0702714
dc.identifierMon.Not.Roy.Astron.Soc.Lett.378:L11-L15,2007
dc.identifierdoi:10.1111/j.1745-3933.2007.00309.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/180206
dc.subjectAstrophysics
dc.titleOn the evolution of the Fe abundance and of the Type Ia SN rate in clusters of galaxies
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