TY - JOUR
T1 - A luminous and fast-expanding type Ib supernova SN 2012au
AU - Takaki, Katsutoshi
AU - Kawabata, Koji S.
AU - Yamanaka, Masayuki
AU - Maeda, Keiichi
AU - Tanaka, Masaomi
AU - Akitaya, Hiroshi
AU - Fukazawa, Yasushi
AU - Itoh, Ryosuke
AU - Kinugasa, Kenzo
AU - Moritani, Yuki
AU - Ohsugi, Takashi
AU - Sasada, Mahito
AU - Uemura, Makoto
AU - Ueno, Issei
AU - Ui, Takahiro
AU - Urano, Takeshi
AU - Yoshida, Michitoshi
AU - Nomoto, Ken'Ichi
PY - 2013/8/1
Y1 - 2013/8/1
N2 - We present a set of photometric and spectroscopic observations of a bright Type Ib supernova SN 2012au from -6 days until + 150 days after maximum. The shape of its early R-band light curve is similar to that of an average Type Ib/c supernova. The peak absolute magnitude is MR = -18.7 ± 0.2 mag, which suggests that this supernova belongs to a very luminous group among Type Ib supernovae. The line velocity of He I λ5876 is about 15,000 km s-1 around maximum, which is much faster than that in a typical Type Ib supernova. From the quasi-bolometric peak luminosity of (6.7 ± 1.3) × 1042 erg s-1, we estimate the 56Ni mass produced during the explosion as 0.30 M. We also give a rough constraint to the ejecta mass 5-7 M and the kinetic energy (7-18) × 1051 erg. We find a weak correlation between the peak absolute magnitude and He I velocity among Type Ib SNe. The similarities to SN 1998bw in the density structure inferred from the light-curve model as well as the large peak bolometric luminosity suggest that SN 2012au had properties similar to energetic Type Ic supernovae.
AB - We present a set of photometric and spectroscopic observations of a bright Type Ib supernova SN 2012au from -6 days until + 150 days after maximum. The shape of its early R-band light curve is similar to that of an average Type Ib/c supernova. The peak absolute magnitude is MR = -18.7 ± 0.2 mag, which suggests that this supernova belongs to a very luminous group among Type Ib supernovae. The line velocity of He I λ5876 is about 15,000 km s-1 around maximum, which is much faster than that in a typical Type Ib supernova. From the quasi-bolometric peak luminosity of (6.7 ± 1.3) × 1042 erg s-1, we estimate the 56Ni mass produced during the explosion as 0.30 M. We also give a rough constraint to the ejecta mass 5-7 M and the kinetic energy (7-18) × 1051 erg. We find a weak correlation between the peak absolute magnitude and He I velocity among Type Ib SNe. The similarities to SN 1998bw in the density structure inferred from the light-curve model as well as the large peak bolometric luminosity suggest that SN 2012au had properties similar to energetic Type Ic supernovae.
KW - supernovae: individual (SN 2012au)
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U2 - 10.1088/2041-8205/772/2/L17
DO - 10.1088/2041-8205/772/2/L17
M3 - Article
AN - SCOPUS:84880586619
VL - 772
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
IS - 2
M1 - L17
ER -