发光的IIN型超新星SN 2017 hcc：红外明亮，X射线和无线电微弱
The luminous Type IIN supernova SN 2017hcc: Infrared bright, X-ray and radio faint
摘要：
利用Chandra X射线望远镜和Swift上的X射线望远镜（Swift-XRT）在X射线波段、Spitzer和TripleSpec光谱仪在近红外和中红外波段以及Karl G. Jansky甚大天线阵（VLA）用于无线电频段。X射线观测涵盖了29至1310天的时间，第一次X射线探测是在第727天。随后，从第1000天起，在VLA无线电波段检测到SN。虽然无线电数据是稀疏的，同步自吸收是明确排除的无线电吸收机制。近红外和中红外的观测表明，后期的红外发射占主导地位的光谱能量分布。\snhcc \的早期性质与冲击波爆发进入致密质量损失区相一致，$\dot M \sim 0.1 M_\odot \rm yr^{-1}$持续了十年。在几个100天，质量损失率下降到$\sim 0.02 M_\odot \rm yr^{-1}$，从占主导地位的红外光度确定。此外，无线电数据还使我们能够计算出大约1000天的质量损失率，这比热辐射峰值附近的质量损失率估计值小两个数量级。这些值表明，SN祖经历了一个增强的质量损失事件前十年的爆炸。在简单的模型中，红外线和X射线的亮度之比很高，这是不对称的星周区域的可能证据。
英文摘要：
We present multiwavelength observations of supernova (SN) 2017hcc with the Chandra X-ray telescope and the X-ray telescope onboard Swift (Swift-XRT) in X-ray bands, with the Spitzer and the TripleSpec spectrometer in near-infrared (IR) and mid-IR bands and with the Karl G. Jansky Very Large Array (VLA) for radio bands. The X-ray observations cover a period of 29 to 1310 days, with the first X-ray detection on day 727 with the Chandra. The SN was subsequently detected in the VLA radio bands from day 1000 onwards. While the radio data are sparse, synchrotron-self absorption is clearly ruled out as the radio absorption mechanism. The near- and the mid-IR observations showed that late time IR emission dominates the spectral energy distribution. The early properties of \snhcc\ are consistent with shock breakout into a dense mass-loss region, with $\dot M \sim 0.1 M_\odot \rm yr^{-1}$ for a decade. At few 100 days, the mass-loss rate declined to $\sim 0.02 M_\odot \rm yr^{-1}$, as determined from the dominant IR luminosity. In addition, radio data also allowed us to calculate a mass-loss rate at around day 1000, which is two orders of magnitude smaller than the mass-loss rate estimates around the bolometric peak. These values indicate that the SN progenitor underwent an enhanced mass-loss event a decade before the explosion. The high ratio of IR to X-ray luminosity is not expected in simple models and is possible evidence for an asymmetric circumstellar region.
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