The Type I[CLC]c[/CLC] Hypernova SN 2002[CLC]ap[/CLC]

P. A. Mazzali(Tokyo University of Science), J. Deng(Tokyo University of Science), Keiichi Maeda(The University of Tokyo), K. Nomoto(Tokyo University of Science), Hideyuki Umeda(Tokyo University of Science), K. Hatano(Tokyo University of Science), K. Iwamoto(Nihon University), Yuzuru Yoshii(Tokyo University of Science), Yukiyasu Kobayashi(National Astronomical Observatory of Japan), Takeo Minezaki(The University of Tokyo), Mamoru Doi(The University of Tokyo), Keigo Enya(The University of Tokyo), Hiroyuki Tomita(The University of Tokyo), S. J. Smartt(University of Cambridge), K. Kinugasa(Gunma Astronomical Observatory), Hideyo Kawakita(Gunma Astronomical Observatory), K. Ayani(Bisei Astronomical Observatory), Tetsuya Kawabata(Bisei Astronomical Observatory), H. Yamaoka(Kyushu University), Y. Qiu(Chinese Academy of Sciences), Kentaro Motohara(The University of Tokyo), C. Gerardy(Dartmouth College), R. Fesen(Dartmouth College), Koji S. Kawabata(National Astronomical Observatory of Japan), Masanori Iye(The Graduate University for Advanced Studies, SOKENDAI), Nobunari Kashikawa(National Astronomical Observatory of Japan), George Kosugi(Subaru (Japan)), Youichi Ohyama(Subaru (Japan)), Masahide Takada‐Hidai(Tokai University), Gang Zhao(Chinese Academy of Sciences), R. Chornock(University of California, Berkeley), A. V. Filippenko(University of California, Berkeley), S. Benetti(Osservatorio Astronomico di Padova), M. Turatto(Osservatorio Astronomico di Padova)
The Astrophysical Journal
June 10, 2002
10.1086/341504
Cited by 307Open Access
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Abstract

Photometric and spectroscopic data of the energetic Type Ic supernova (SN) 2002ap are presented, and the properties of the SN are investigated through models of its spectral evolution and its light curve. The SN is spectroscopically similar to the hypernova SN 1997ef. However, its kinetic energy [~(4-10) ? 1051 ergs] and the mass ejected (2.5-5 M?) are smaller, resulting in a faster evolving light curve. The SN synthesized ~0.07 M? of 56Ni, and its peak luminosity was similar to that of normal SNe. Brightness alone should not be used to define a hypernova, whose defining character, namely very broad spectral features, is the result of high kinetic energy. The likely main-sequence mass of the progenitor star was 20-25 M?, which is also lower than that of both hypernovae SN 1997ef and SN 1998bw. SN 2002ap appears to lie at the low-energy and low-mass end of the hypernova sequence as it is known so far. Observations of the nebular spectrum, which is expected to dominate by the summer of 2002, are necessary to confirm these values.

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