Measured metallicities at the sites of nearby broad-lined type Ic supernovae and implications for the supernovae gamma-ray burst connection
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Modjaz, M.
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Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Modjaz, M.
[1
,2
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Kewley, L.
[3
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Kirshner, R. P.
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Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Kirshner, R. P.
[1
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Stanek, K. Z.
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Ohio State Univ, Dept Astron, Columbus, OH 43210 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Stanek, K. Z.
[4
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Challis, P.
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Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Challis, P.
[1
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Garnavich, P. M.
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Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Garnavich, P. M.
[5
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Greene, J. E.
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Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Greene, J. E.
[6
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Kelly, P. L.
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Kali Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Kelly, P. L.
[7
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Prieto, J. L.
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Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USAHarvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
Prieto, J. L.
[5
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机构:
[1] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[2] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA
[3] Univ Hawaii, Honolulu, HI 96822 USA
[4] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA
[5] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA
[6] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA
[7] Kali Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA
We compare the chemical abundances at the sites of 12 nearby (z < 0.14) Type Ic supernovae (SN Ic) that showed broad lines, but had no observed gamma-ray burst (GRB), with the chemical abundances in five nearby (z < 0.25) galaxies at the sites of GRBs where broad-lined SN Ic were seen after the fireball had faded. It has previously been noted that GRB hosts are low in luminosity and low in their metal abundances. If low metallicity is sufficient to force the evolution of massive stars to end their lives as GRBs with an accompanying broad-lined SN Ic, then we would expect higher metal abundances for the broad-lined SN Ic that have no detected GRBs. This is what we observe, and this trend is independent of the choice of metallicity calibration we adopt and the mode of SN survey that found the broad-lined SN Ic. A unique feature of this analysis is that we present new spectra of the host galaxies and analyze all measurements of both samples in the same set of methods, using the galaxy emission-line measurements corrected for extinction and stellar absorption, via independent metallicity diagnostics of Kewley & Dopita, McGaugh, and Pettini & Pagel. In our small sample, the boundary between galaxies that have GRBs accompanying their broad-lined SN Ic and those that have broad-lined SN Ic without GRBs lies at an oxygen abundance of 12 + log(O/H)(KD02) similar to 8.5, which corresponds to 0.2-0.6 Z(circle dot) depending on the adopted metallicity scale and solar abundance value. Even when we limit the comparison to SN Ic that were found in untargeted supernova surveys, the environment of every broad-lined SN Ic that had no GRB is more metal rich than the site of any broad-lined SN Ic where a GRB was detected.