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Abundance ratios in hierarchical galaxy formation

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In models of hierarchical galaxy formation ellipticals form through the merging of smaller disk systems (e.g., Kauffmann, White and Guiderdoni,1993). Such models predict that galaxies in low-density environments form later than their counterparts in clusters, and more massive galaxies form later (Kauffmann, 1996). Here we present simulations based on semi-analytic models that include the chemical enrichment of the elements magnesium andiron. The chemical evolution code is described in Thomas, Greggio and Bender(1998, 1999). The results are: 1) The Mg/Fe predicted for elliptical galaxies does not agree with the values derived from observations. 2) The most luminous (and massive) ellipticals have the lowest Mg/Fe, in conflict with the observational evidence. 3) Galaxies in looser environments exhibit lower Mg/Fe ratios. 4) Bulges are most α-enhanced independent of the environment. For more details I refer the reader to Thomas (1999) and Thomas and Kauffmann (1999).
Original languageEnglish
Pages (from-to)209-209
JournalAstrophysics and Space Science
Volume277
Issue number1 Supp
DOIs
Publication statusPublished - 1999

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