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II型超新星的晚期光变曲线：SNe的物理性质及其环境

Late-time Light Curves of Type II Supernovae: Physical Properties of SNe and Their Environment

Masaaki Otsuka, Margaret Meixner, Nino Panagia, Joanna Fabbri, Michael J. Barlow, Geoffrey C. Clayton, Joseph S. Gallagher, Ben E. K. Sugerman, Roger Wesson, Je… 展开作者

Masaaki Otsuka, Margaret Meixner, Nino Panagia, Joanna Fabbri, Michael J. Barlow, Geoffrey C. Clayton, Joseph S. Gallagher, Ben E. K. Sugerman, Roger Wesson, Jennifer E. Andrews, Barbara Ercolano, Douglas Welch

备注：
We corrected the 56Ni mass of SN2005cs and Figures 8 (a) and 8 (c)
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摘要：

利用哈勃望远镜（HST）、双子座北座望远镜（Gemini north）和WIYN望远镜对SNe 1999 bw、2002 hh、2003 gd、2004 et、2005 cs和2006 bc等6颗核心坍缩超新星的BVRIJHK波段测光结果进行了观测。我们还展示了超新星冒名顶替者SN 2008 S到第575天的JHK光变曲线。在我们总共43次HST观测中，有36次观测成功地探测到了来自SNe的光，并测量了所有目标的星等。HST观测结果显示，在第1520天SN 2003 gd周围和第1717天SN 2002 hh周围存在分辨散射光回波。我们的双子座和WIYN观测也发现了SNe 2002 hh和2004 et。结合我们的数据与以前公布的数据，我们显示VRIJHK波段光变曲线和估计下降幅度率在每个波段在4个不同的阶段。我们之前对这些光变曲线和其他数据的研究表明，尘埃在我们的目标中形成的时间是300-400天，支持SN尘埃形成理论。在本文中，我们专注于其他物理性质的晚时间光变曲线。我们用SN 1987 A作为标准（7.5 x 10 ^{-2} Msun），从每个目标在150-300天内的辐射热光变曲线中估算了56 Ni的质量（0.5 -14 x 10 ^{-2} Msun）。SNe 2002 hh、2003 gd、2004 et和2006 bc的光变曲线变平或有时增加的光通量表明光回波的存在。我们估计了产生光回波的物质的星周氢密度，发现SN 2002 hh被相对致密的物质（n（H）>400 cm^{-3}）包围，而SNe 2003 gd和2004 et的密度更典型的星际介质（~1 cm^{-3}）。56 Ni的质量似乎与原始质量有很好的相关性，斜率为0.31 x 10^{-2}，支持Maeda等人（2010）之前的工作，他们专注于更大质量的II型SNe。尘埃质量似乎并不与祖质量。

英文摘要：

We present BVRIJHK band photometry of 6 core-collapse supernovae, SNe 1999bw, 2002hh, 2003gd, 2004et, 2005cs, and 2006bc measured at late epochs (>2 yrs) based on Hubble Space Telescope (HST), Gemini north, and WIYN telescopes. We also show the JHK lightcurves of a supernova impostor SN 2008S up to day 575. Of our 43 HST observations in total, 36 observations are successful in detecting the light from the SNe alone and measuring magnitudes of all the targets. HST observations show a resolved scattered light echo around SN 2003gd at day 1520 and around SN 2002hh at day 1717. Our Gemini and WIYN observations detected SNe 2002hh and 2004et, as well. Combining our data with previously published data, we show VRIJHK-band lightcurves and estimate decline magnitude rates at each band in 4 different phases. Our prior work on these lightcurves and other data indicate that dust is forming in our targets from day ~300-400, supporting SN dust formation theory. In this paper we focus on other physical properties derived from the late time light curves. We estimate 56Ni masses for our targets (0.5-14 x 10^{-2} Msun) from the bolometric lightcurve of each for days ~150-300 using SN 1987A as a standard (7.5 x 10^{-2} Msun). The flattening or sometimes increasing fluxes in the late time light curves of SNe 2002hh, 2003gd, 2004et and 2006bc indicate the presence of light echos. We estimate the circumstellar hydrogen density of the material causing the light echo and find that SN 2002hh is surrounded by relatively dense materials (n(H) >400 cm^{-3}) and SNe 2003gd and 2004et have densities more typical of the interstellar medium (~1 cm^{-3}). The 56Ni mass appears well correlated with progenitor mass with a slope of 0.31 x 10^{-2}, supporting the previous work by Maeda et al. (2010), who focus on more massive Type II SNe. The dust mass does not appear to be correlated with progenitor mass.

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