SN 2002 hh的后期光谱：一个没有激波相互作用的连续可见光回波
Late-time spectroscopy of SN 2002hh: A continued visible light echo with no shock interaction yet
摘要：
超新星（SN）2002 hh在核心坍缩的超新星中是不寻常的，因为它是高度红化的，并且由于其星周介质（CSM）中的辐射加热尘埃而显示出明亮的红外线（IR）过量。对造成红外回波的尘埃质量的估计表明，在恒星0.26 pc范围内存在一个巨大的壳层。对于5，000 - 10，000 km/s的速度，这种材料应该在晚些时候，大约在爆炸后12年开始受到SN冲击波的撞击。我们已经获得了深晚时间光谱与MMT蓝通道摄谱仪搜索任何正在进行的冲击相互作用的光谱特征。在我们的数据中将检测到强度相当于SN 1987 A与赤道环碰撞的相互作用。然而，在这里报道的光谱，我们没有检测到强CSM相互作用的明显迹象，相反的期望的基础上报告的尘埃壳半径。然而，我们确实检测到了与旧SN相关的发射，我们发现光谱中的宽线表明持续的反射光回波，这与II-P型事件峰值亮度的光谱相似。
英文摘要：
Supernova (SN) 2002hh was unusual among core-collapse SNe because it was highly reddened, and displayed a bright infrared (IR) excess due to radiatively heated dust in its circumstellar medium (CSM). Estimates for the mass of dust responsible for the IR echo suggested the presence of a massive shell within 0.26 pc of the star. For a velocity of 5000 - 10000 km/s, this material should be hit by the SN blast wave at late times, starting at roughly 12 years post-explosion. We have obtained deep late-time spectra with the MMT Blue Channel spectrograph to search for any spectral signatures of ongoing shock interaction. Interaction with a strength comparable to SN 1987A's collision with the equatorial ring would be detected in our data. However, in the spectra reported here, we do not detect clear signs of strong CSM interaction, contrary to expectations based on the reported radii of the dust shell. We do, however, detect emission associated with the old SN, and we find that the broad lines in the spectrum indicate a continuation of an ongoing reflected light echo, which appears similar to the spectrum at peak luminosity for this Type II-P event.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
