EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc-猫眼课题宝

DOI：

10.1088/0004-637x/707/2/l118

发表时间：

2009-08

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

M. Yamanaka;K. Kawabata;K. Kinugasa;Masaomi Tanaka;A. Imada;K. Maeda;K. Nomoto;Akira Arai;S. Chiyonobu;Y. Fukazawa;Osamu Hashimoto;Satoshi Honda;Y. Ikejiri;R. Itoh;Yukiko Kamata;N. Kawai;T. Komatsu;K. Konishi;D. Kuroda;H. Miyamoto;S. Miyazaki;O. Nagae;H. Nakaya;T. Ohsugi;T. Omodaká;Nobuyuki Sakai;M. Sasada;Mariko Suzuki;H. Taguchi;H. Takahashi;Hiroyuki Tanaka;M. Uemura;Takuya Yamashita;K. Yanagisawa;Michitoshi Yoshida

我们目前的光学和近红外波长的非常明亮的Ia型超新星（SN Ia）2009dc的早期阶段的观测。光变曲线的衰减速率为Δ m 15（B）= 0.65 ± 0.03，是Ia超新星中衰减速率最慢的一个。如果假设没有宿主消光，V波段的峰值绝对星等估计为MV = −19.90 ± 0.15等。如果我们假设母星的消光为AV = 0.29等，则它的亮度为MV = −20.19 ± 0.19等。SN 2009dc与SN 2003fg和2006gz一样，属于超新星Ia中最明亮的一类。我们的JHKs波段测光表明，这个SN也是近红外波长中最明亮的SNe Ia之一。我们估计，在无宿主绝灭的情况下，56 Ni的喷射质量为1.2 ± 0.3 M（在AV = 0.29等的宿主绝灭情况下，喷射质量为1.6 ± 0.4 M）。C ii λ6580的吸收线在最大亮度之后一周内仍然可见，与SN 2006 gz的早期消失形成对比。Si ii λ6355的线速度在最大值附近约为8000 km s−1，比SN 2006gz慢得多。在最大值附近，C ii线的速度类似于或略小于Si ii线的速度。碳线的存在表明爆炸后留下了厚厚的未燃烧的C+O层。Tanaka等人的光谱偏振观测表明，爆炸几乎是球形的。这些观测事实表明SN 2009 dc是一个超克拉塞卡质量的SN Ia。

We present early phase observations in optical and near-infrared wavelengths for the extremely luminous Type Ia supernova (SN Ia) 2009dc. The decline rate of the light curve is Δm15(B) = 0.65 ± 0.03, which is one of the slowest among SNe Ia. The peak V-band absolute magnitude is estimated to be MV = −19.90 ± 0.15 mag if no host extinction is assumed. It reaches MV = −20.19 ± 0.19 mag if we assume the host extinction of AV = 0.29 mag. SN 2009dc belongs to the most luminous class of SNe Ia, like SNe 2003fg and 2006gz. Our JHKs-band photometry shows that this SN is also one of the most luminous SNe Ia in near-infrared wavelengths. We estimate the ejected 56Ni mass of 1.2 ± 0.3 M☉ for the no host extinction case (and of 1.6 ± 0.4 M☉ for the host extinction of AV = 0.29 mag). The C ii λ6580 absorption line remains visible until a week after the maximum brightness, in contrast to its early disappearance in SN 2006gz. The line velocity of Si ii λ6355 is about 8000 km s−1 around the maximum, being considerably slower than that of SN 2006gz. The velocity of the C ii line is similar to or slightly less than that of the Si ii line around the maximum. The presence of the carbon line suggests that the thick unburned C+O layer remains after the explosion. Spectropolarimetric observations by Tanaka et al. indicate that the explosion is nearly spherical. These observational facts suggest that SN 2009dc is a super-Chandrasekhar mass SN Ia.

EARLY PHASE OBSERVATIONS OF EXTREMELY LUMINOUS TYPE Ia SUPERNOVA 2009dc

文献摘要

被引文献

相似文献