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Mass and metallicity constraints on supernova progenitors derived from integral field spectroscopy of the environment

Published online by Cambridge University Press:  05 September 2012

Hanindyo Kuncarayakti ,
Mamoru Doi ,
Greg Aldering ,
Nobuo Arimoto ,
Keiichi Maeda ,
Tomoki Morokuma ,
Rui Pereira ,
Tomonori Usuda  and
Yasuhito Hashiba
Hanindyo Kuncarayakti
Affiliation:
Institute of Astronomy, Graduate School of Science, the University of Tokyo2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan email: [email protected]
Mamoru Doi
Affiliation:
Institute of Astronomy, Graduate School of Science, the University of Tokyo2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan email: [email protected]
Greg Aldering
Affiliation:
Physics Division, Lawrence Berkeley National Laboratory 1 Cyclotron Road, Berkeley, CA 94720, USA
Nobuo Arimoto
Affiliation:
National Astronomical Observatory of Japan 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
Keiichi Maeda
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe, the University of Tokyo 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
Tomoki Morokuma
Affiliation:
Institute of Astronomy, Graduate School of Science, the University of Tokyo2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan email: [email protected]
Rui Pereira
Affiliation:
CNRS/IN2P3, Institut de Physique Nucléaire de Lyon 4 Rue Enrico Fermi, 69622 Villeurbanne Cedex, France
Tomonori Usuda
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan 650 North A'ohoku Place, Hilo, HI 96720, USA
Yasuhito Hashiba
Affiliation:
Institute of Astronomy, Graduate School of Science, the University of Tokyo2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan email: [email protected]
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Abstract

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We have obtained optical integral field spectroscopy of the explosion sites of more than 25 nearby type-IIP/IIL/Ib/Ic supernovae using UH88/SNIFS, and additionally Gemini/GMOS IFU. This technique enables us to obtain both spatial and spectral information of the immediate environment of the supernovae. Using strong line method we measured the metallicity of the star cluster present at the explosion site, presumably the coeval parent stellar population of the supernova progenitor, and comparison with simple stellar population models gives age estimate of the cluster. With this method we were able to put constraints on the metallicity and age of the progenitor star. The age, i.e. lifetime, of the progenitor corresponds to the initial mass of the star. By far this is the most direct measurement of supernova progenitor metallicity and, if the cluster-progenitor association is confirmed, provides reliable determination of the initial mass of supernova progenitor stars.

Keywords

stars: supernovae
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 343 - 344
Copyright
Copyright © International Astronomical Union 2012

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