正常Ia型SN 2003 hv输出到非常晚的阶段
The normal Type Ia SN 2003hv out to very late phases
摘要：
SN 2003 hv的一个广泛的数据集，涵盖了从最大光到+786天的通量演变。这些数据与已发表的星云相红外光谱相结合，并将观测结果与模型光变曲线和合成星云光谱进行了比较。SN 2003 hv是一颗正常的Ia型超新星，其光度和光谱特性与B波段的衰减率参数一致，Δ m_15 = 1.61 +- 0.02。在星云相光谱中最孤立的[Fe II]线的蓝移似乎与在类似时期的红外线中观察到的一致。在后期，有一个普遍的颜色演变从光学向近红外波段。我们提出了有史以来最新的探测超新星Ia在近红外哈勃太空望远镜的图像。对紫外/光学/红外（UVOIR）光变曲线的研究表明，相当大一部分通量在后期“丢失”。在最大亮度过去300-700天之间，UVOIR光变曲线随着放射性Co 56的衰变而线性下降，假设正电子被完全和瞬时捕获。在700天，我们检测到光学波段的下降可能放缓，主要是在V波段。这些数据与一场戏剧性的红外灾难不一致。然而，红外灾难发生在350天前的dennis区域的想法可以解释从UVOIR波长的通量和平顶的近红外轮廓的丢失。我们认为，这样的情况是可能的，如果喷出物是cloudly。观测结果表明，正电子很可能被困在喷出物中。
英文摘要：
An extensive dataset for SN 2003hv that covers the flux evolution from maximum light to day +786 is presented. The data are combined with published nebular-phase infrared spectra, and the observations are compared to model light curves and synthetic nebular spectra. SN 2003hv is a normal Type Ia supernova (SN Ia) with photometric and spectroscopic properties consistent with its rarely observed B-band decline-rate parameter, Delta m_15 = 1.61 +- 0.02. The blueshift of the most isolated [Fe II] lines in the nebular-phase optical spectrum appears consistent with those observed in the infrared at similar epochs. At late times there is a prevalent color evolution from the optical toward the near-infrared bands. We present the latest-ever detection of a SN Ia in the near-infrared in Hubble Space Telescope images. The study of the ultraviolet/optical/infrared (UVOIR) light curve reveals that a substantial fraction of the flux is "missing" at late times. Between 300-700 days past maximum brightness, the UVOIR light curve declines linearly following the decay of radioactive Co56, assuming full and instantaneous positron trapping. At 700 days we detect a possible slowdown of the decline in optical bands, mainly in the V band. The data are incompatible with a dramatic infrared catastrophe. However, the idea that an infrared catastrophe occurred in the densest regions before 350 days can explain the missing flux from the UVOIR wavelengths and the flat-topped profiles in the near-infrared. We argue that such a scenario is possible if the ejecta are clumpy. The observations suggest that positrons are most likely trapped in the ejecta.
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