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Galactic chemical evolution and GRB host identification

Published online by Cambridge University Press:  27 October 2016

Francesca Matteucci  and
Valentina Grieco
Francesca Matteucci
Affiliation:
Dipartimento di Fisica, Universita' di Trieste, Via G.B. Tiepolo, 11 34131TriesteItaly email: [email protected]
Valentina Grieco
Affiliation:
Dipartimento di Fisica, Universita' di Trieste, Via G.B. Tiepolo, 11 34131TriesteItaly email: [email protected]
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Abstract

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We describe a method to identify GRB host galaxies by means of their chemical abundances. We apply this method to three GRB hosts by comparing detailed chemical evolution models, including dust, of galaxies of different morphological type to observed abundance ratios. We conclude that none of them is likely to be a dwarf irregular galaxy, as it is believed for the majority of GRB hosts, but rather two of them (GRB081008 and GRB120327A) are likely to be spirals and the third is likely to be an elliptical (GRB120815). In addition, we have derived their chemical ages: in particular, the elliptical host is only 15 Myr old, while the other two hosts are 50 Myr (GRB120327A) and 320 Myr (GRB130815).

Keywords

galaxies: evolutiongamma rays: bursts
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 255 - 256
Copyright
Copyright © International Astronomical Union 2016 

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