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arXiv 0705.3478astro-ph
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SN 2006 bp：探测II-P型超新星的激波爆发

SN 2006bp: Probing the Shock Breakout of a Type II-P Supernova

Robert M. Quimby, J. Craig Wheeler, Peter Höflich, Carl W. Akerlof, Peter J. Brown, Eli S. Rykoff

备注：
ApJ accepted, 43 pages
发表信息：
Astrophys.J.666:1093-1107,2007
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摘要：

本文介绍了II-P型SN 2006 bp爆炸后前11个月的HET光谱学和未经过滤的ROTSE-III光度学。在发现前几天的通量极限与最初的快速增亮相结合，表明超新星是在冲击爆发后几个小时才首次被发现的。爆发后约2天获得的光谱表现出狭窄的发射线，对应于HeII 4200，HeII 4686和CIV 5805在休息帧，这些功能坚持在第二次观察后获得5小时;然而，这些发射线没有检测到第二天晚上，也没有在随后的观察。我们认为，这些线从靠近爆炸现场的材料发出，可能在外层的祖先，已被电离的高能量光子在冲击爆发释放。在+2和+3天光谱中，在4450 A附近观察到P-Cygni轮廓。以前的研究认为这一特征是由于高速的H-β，但我们讨论的可能性，这一配置文件，而不是由于HeII 4687。进一步的HET观测（共14个夜晚）涵盖了爆发后73天内整个测光平台的光谱演化以及+340天左右的星云阶段，并推导了关键特征的膨胀速度。在+121天和+335天之间，未过滤的光变曲线的测量衰减斜率为0.0073 +/- 0.0004 mag/天，这比56 Co的衰减率明显慢。我们将我们的HET测量结果与已公布的X射线，紫外线和光学数据相结合，以获得通过第+60天的准测辐射热光曲线。我们看到在最初的25天里有一个缓慢的冷却，但没有早期尖峰的迹象;任何来自冲击爆发的这样的特征都必须持续不到1天。[删节]

英文摘要：

HET optical spectroscopy and unfiltered ROTSE-III photometry spanning the first 11 months since explosion of the Type II-P SN 2006bp are presented. Flux limits from the days before discovery combined with the initial rapid brightening suggest the supernova was first detected just hours after shock breakout. Optical spectra obtained about 2 days after breakout exhibit narrow emission lines corresponding to HeII 4200, HeII 4686, and CIV 5805 in the rest frame, and these features persist in a second observation obtained 5 hours later; however, these emission lines are not detected the following night nor in subsequent observations. We suggest that these lines emanate from material close to the explosion site, possibly in the outer layers of the progenitor that have been ionized by the high energy photons released at shock breakout. A P-Cygni profile is observed around 4450 A in the +2 and +3 day spectra. Previous studies have attributed this feature to high velocity H-beta, but we discuss the possibility that this profile is instead due to HeII 4687. Further HET observations (14 nights in total) covering the spectral evolution across the photometric plateau up to 73 days after breakout and during the nebular phase around day +340 are presented, and expansion velocities are derived for key features. The measured decay slope for the unfiltered light curve is 0.0073 +/- 0.0004 mag/day between days +121 and +335, which is significantly slower than the decay of rate 56Co. We combine our HET measurements with published X-ray, UV, and optical data to obtain a quasi-bolometric light curve through day +60. We see a slow cooling over the first 25 days, but no sign of an early sharp peak; any such feature from the shock breakout must have lasted less than ~1 day.[ABRIDGED]

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