Niino, Y. 2011 长暴宿主星系的金属丰度

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Title:		Revisiting the metallicity of long-duration gamma-ray burst host galaxies: the role of chemical inhomogeneity within galaxies
Authors:		Niino, Y.
Affiliation:		AA(Division of Optical & Infrared Astronomy, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomy, School of Science, Kyoto University, Kitashirakawa-Oiwakecho, Sakyo-ku, Kyoto 606-8502, Japan)
Publication:		Monthly Notices of the Royal Astronomical Society, Volume 417, Issue 1, pp. 567-572. (MNRAS Homepage)
Publication Date:		10/2011
Origin:		WILEY
Astronomy Keywords:		galaxies: abundances, gamma-ray burst: general
Abstract Copyright:		© 2011 The Author Monthly Notices of the Royal Astronomical Society © 2011 RAS
DOI:		10.1111/j.1365-2966.2011.19299.x
Bibliographic Code:		2011MNRAS.417..567N

Abstract

We predict the metallicity probability distribution function (PDF) of long gamma-ray burst (GRB) host galaxies at low redshifts (z≲ 0.3) when GRBs occur only in low-metallicity environments, assuming empirical formulations of galaxy properties. We discuss the contribution of high-metallicity galaxies to the cosmic rate of low-metallicity GRBs, taking the internal dispersion of metallicity within each galaxy into account. Assuming that GRBs trace low-metallicity star formation <Z_crit: 12+log₁₀(O/H) = 8.2, we find that GRB host galaxies may have systematically higher metallicity than GRB progenitors. Furthermore, we expect >rsim10 per cent of the host galaxies to have 12+log₁₀(O/H) > 8.8, if galaxies have an internal dispersion of metallicity comparable to that observed in the Milky Way. Our results show that the low-metallicity scenario of GRB progenitors can be reconciled with recent discoveries of the high-metallicity host galaxies of GRBs. We also show a possible bimodality in the host metallicity PDF that results from the single-progenitor model of GRBs. If found in future observations, the bimodality might be a clue to constrain the nature of GRB progenitors.

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