Probing Star Formation Timescales in Elliptical Galaxies

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dc.creatorThomas, Daniel
dc.creatorKauffmann, Guinevere
dc.date1999-06-12
dc.date.accessioned2026-07-07T02:31:59Z
dc.date.available2026-07-07T02:31:59Z
dc.descriptionIn models of galaxy formation in a hierarchical Universe, elliptical galaxies form through the merging of smaller disk systems. These models yield a number of testable predictions if reliable techniques for determining the relative ages and compositions of the stellar populations of different galaxies can be found: 1) ellipticals in low-density environments form later than ellipticals in clusters, 2) more massive ellipticals form later, 3) more massive ellipticals form in dissipationless mergers from disk galaxies with low gas content. While colours and the Balmer line strengths of galaxies can be used to infer the average ages of the stellar populations of ellipticals, alpha/Fe element ratios carry information about the timescale over which star formation took place. Here we present preliminary results from semi-analytic models for the distribution of Mg/Fe ratios in galaxies as a function of morphological type, luminosity and environment.
dc.description11 pages, 5 figures, to appear in the PASP Conference Proccedings series of the Workshop "Spectrophotometric dating of stars and galaxies", Annapolis, Maryland (USA), eds. I. Hubeny, S. Heap, and R. Cornett
dc.identifierhttps://arxiv.org/abs/astro-ph/9906216
dc.identifierhttp://arxiv.org/abs/astro-ph/9906216
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/14354
dc.subjectAstrophysics
dc.titleProbing Star Formation Timescales in Elliptical Galaxies
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