A SEARCH FOR INFRARED EMISSION FROM CORE-COLLAPSE SUPERNOVAE AT THE TRANSITIONAL PHASE
A SEARCH FOR INFRARED EMISSION FROM CORE-COLLAPSE SUPERNOVAE AT THE TRANSITIONAL PHASE
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DOI：
10.1088/0004-637x/749/2/173
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发表时间：
2012-02
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通讯作者：
Masaomi Tanaka;T. Nozawa;I. Sakon;T. Onaka;K. Arimatsu;R. Ohsawa;K. Maeda;T. Wada;H. Matsuhara;H. Kaneda
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作者：
Masaomi Tanaka;T. Nozawa;I. Sakon;T. Onaka;K. Arimatsu;R. Ohsawa;K. Maeda;T. Wada;H. Matsuhara;H. Kaneda
大多数超新星 (SN) 爆炸的观测研究仅限于我们银河系或非常邻近的星系的早期阶段（100 年）。这两个时期之间的超新星，我们称之为“过渡”阶段，除了包括大麦哲伦星云中的 SN 1987A 在内的几个河外超新星外，还没有被详细探索过。我们通过多种机制对红外 (IR) 粉尘排放进行了理论预测； SN喷射物中形成的尘埃的发射、星周（CS）和星际（IS）尘埃的光回波以及冲击的CS尘埃的发射。我们利用 AKARI 卫星和 Spitzer 获取的数据，搜索附近星系 NGC 1313、NGC 6946 和 M101 过渡阶段的六个核心塌缩超新星的红外发射。在六个目标中，我们在 NGC 1313 中检测到了 SN 1978K 的发射。SN 1978K 与 1.3 × 10−3 M☉ 的硅酸盐尘埃有关。我们表明，在多种机制中，冲击的 CS 尘埃是解释 SN 1978K 观测到的红外发射的最可能的发射源。未检测到其他五个物体的红外发射。我们目前的观测对 >1038 erg s−1 的红外光度敏感，并且未检测到 SN 1962M 排除了受冲击的 CS 尘埃的存在，气体质量损失率高达 ∼10−4 M☉ yr−1。未来红外卫星对过渡阶段超新星的观测将填补超新星10-100年龄红外观测的空白，并为研究超新星前身的CS和IS环境以及可能的超新星尘埃形成提供新的机会。
Most of the observational studies of supernova (SN) explosions are limited to early phases (100 yr) in our Galaxy or very nearby galaxies. SNe at the epoch between these two, which we call the “transitional” phase, have not been explored in detail except for several extragalactic SNe including SN 1987A in the Large Magellanic Cloud. We present theoretical predictions for the infrared (IR) dust emissions by several mechanisms; emission from dust formed in the SN ejecta, light echo by circumstellar (CS) and interstellar (IS) dust, and emission from shocked CS dust. We search for IR emission from six core-collapse SNe at the transitional phase in the nearby galaxies NGC 1313, NGC 6946, and M101 by using the data taken with the AKARI satellite and Spitzer. Among six targets, we detect the emission from SN 1978K in NGC 1313. SN 1978K is associated with 1.3 × 10−3 M☉ of silicate dust. We show that, among several mechanisms, the shocked CS dust is the most probable emission source to explain the IR emission observed for SN 1978K. IR emission from the other five objects is not detected. Our current observations are sensitive to IR luminosity of >1038 erg s−1, and the non-detection of SN 1962M excludes the existence of the shocked CS dust for a high gas mass-loss rate of ∼10−4 M☉ yr−1. Observations of SNe at the transitional phase with future IR satellites will fill the gap of IR observations of SNe with the age of 10–100 yr, and give a new opportunity to study the CS and IS environments of the progenitor, and possibly dust formation in SNe.