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Metallicities at the Sites of Nearby SN and Implications for the SN-GRB Connection

Published online by Cambridge University Press:  01 December 2007

Maryam Modjaz ,
L. Kewley ,
R. P. Kirshner ,
K. Z. Stanek ,
P. Challis ,
P. M. Garnavich ,
J. E. Greene ,
P. L. Kelly  and
J. L. Prieto
Maryam Modjaz
Affiliation:
UC Berkeley Astronomy Department email: [email protected] Harvard-Smithsonian CfA email: [email protected], [email protected]
L. Kewley
Affiliation:
Department of Astronomy, Univerisity of Hawaii email: [email protected]
R. P. Kirshner
Affiliation:
Harvard-Smithsonian CfA email: [email protected], [email protected]
K. Z. Stanek
Affiliation:
Department of Astronomy, The Ohio State University email: [email protected], [email protected]
P. Challis
Affiliation:
Harvard-Smithsonian CfA email: [email protected], [email protected]
P. M. Garnavich
Affiliation:
Department of Physics, University of Notre Dame email: [email protected]
J. E. Greene
Affiliation:
Department of Astrophysical Sciences, Princeton University email: [email protected]
P. L. Kelly
Affiliation:
Kavli Institute for Particle Astrophysics and Cosmology email: [email protected]
J. L. Prieto
Affiliation:
Department of Astronomy, The Ohio State University email: [email protected], [email protected]
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Abstract

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While the broad-lined Type Ic supernovae (SN Ic-bl) associated with long-duration gamma-ray bursts (GRBs) have been studied, we do not fully understand the conditions that lead to each kind of explosion in a massive star. Here we show clues as to the production mechanism of GRBs by comparing the chemical abundances at the sites of 5 nearby (z < 0.25) broad-lined SN Ic that accompany nearby GRBs with those of 12 nearby (z < 0.14) broad-lined SN Ic that have no observed GRBs. We show that the oxygen abundances at the GRB sites are systematically lower than those found near ordinary broad-lined SN Ic. A unique feature of this analysis is that we present new spectra of the host galaxies and analyze the measurements of both samples in the same set of ways, using 3 independent metallicity diagnostics. We demonstrate that neither SN selection effects (SN found via targeted vs. non-targeted surveys) nor the choice of strong-line metallicity diagnostic can cause the observed trend. Though our sample size is small, the observations are consistent with the hypothesis that low metal abundance is the cause of some massive stars becoming SN-GRB. We derive a cut-off metallicity of 0.2−0.6 Z⊙, with the exact value depending on the adopted metallicity scale and solar abundance value.

Keywords

gamma rays: bursts – supernovae: individual – galaxies: abundances
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S250: Massive Stars as Cosmic Engines , December 2007 , pp. 503 - 508
Copyright
Copyright © International Astronomical Union 2008

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