TYPE Ia SUPERNOVAE STRONGLY INTERACTING WITH THEIR CIRCUMSTELLAR MEDIUM
TYPE Ia SUPERNOVAE STRONGLY INTERACTING WITH THEIR CIRCUMSTELLAR MEDIUM
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DOI：
10.1088/0067-0049/207/1/3
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发表时间：
2013-04
期刊：
影响因子：
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通讯作者：
J. Silverman;P. Nugent;A. Gal-yam;M. Sullivan;D. Howell;A. Filippenko;I. Arcavi;S. Ben-Ami;J. Bloom;S. Cenko;Yi Cao;R. Chornock;K. Clubb;A. Coil;R. Foley;M. Graham;C. Griffith;A. Horesh;M. Kasliwal;S. Kulkarni;D. Leonard;Weidong Li;T. Matheson;Adam A. Miller;M. Modjaz;E. Ofek;Yen-Chen Pan;D. Perley;D. Poznanski;R. Quimby;T. Steele;A. Sternberg;Dong Xu;O. Yaron
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文献类型：
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作者：
J. Silverman;P. Nugent;A. Gal-yam;M. Sullivan;D. Howell;A. Filippenko;I. Arcavi;S. Ben-Ami;J. Bloom;S. Cenko;Yi Cao;R. Chornock;K. Clubb;A. Coil;R. Foley;M. Graham;C. Griffith;A. Horesh;M. Kasliwal;S. Kulkarni;D. Leonard;Weidong Li;T. Matheson;Adam A. Miller;M. Modjaz;E. Ofek;Yen-Chen Pan;D. Perley;D. Poznanski;R. Quimby;T. Steele;A. Sternberg;Dong Xu;O. Yaron
由于Ia型超新星（SNe Ia）在测量宇宙加速方面的实用性，它们可能是SNe中研究得最好的一类，但这些爆炸的祖先系统在很大程度上仍然是一个谜。Ia型超新星的一个罕见的子类显示出与其星周介质（CSM），特别是富含氢的CSM有强烈相互作用的证据;我们将它们称为Ia型超新星-CSM。在第一次系统的搜索这样的系统，我们已经确定了16 SNe Ia-CSM，在这里，我们提出了新的光谱，其中13个。六个SNe Ia-CSM以前已经得到了很好的研究，三个以前是已知的，但在这里是第一次深入分析，七个是新发现的帕洛玛瞬态工厂。所有超新星Ia-CSM的光谱都以Hα辐射为主（宽度约为2000 km s−1），并显示出很大的Hα/Hβ强度比（可能是由于超新星喷出物超越了移动较慢的CSM壳层而碰撞激发了氢）;此外，它们几乎完全没有He i辐射。它们还显示了通过Hα的红翼在最大亮度后75-100天的减少而形成尘埃的可能证据，并且几乎所有的SNe Ia-CSM都表现出来自宿主星系的强烈Na i D吸收。SNe Ia-CSM的绝对星等（未校正主星系消光）为−21.3等，并且在早期似乎有紫外线辐射，在晚期则有强烈的红外线辐射（但没有侦测到射电或X射线辐射）。最后，SNe Ia-CSM的宿主星系都是类似于银河系的晚型螺旋星系，或者是像大麦哲伦云这样的矮不规则星系，这意味着这些天体来自相对年轻的恒星群体。这项工作是迄今为止对SN Ia-CSM类的最详细的分析。
Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the best-studied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogen-rich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by Hα emission (with widths of ∼2000 km s−1) and exhibit large Hα/Hβ intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He i emission. They also show possible evidence of dust formation through a decrease in the red wing of Hα 75–100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na i D absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be −21.3 mag ⩽ MR ⩽ −19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date.