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arXiv 0912.3302astro-ph.CO
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关于II-P型超新星2004 et、2006 my和2006 ov的前身星性质

On the nature of the progenitors of three type II-P supernovae: 2004et, 2006my and 2006ov

R. M. Crockett, S. J. Smartt, A. Pastorello, J. J. Eldridge, A. W. Stephens, J. R. Maund, S. Mattila

备注：
43 pages (pre-print format), 12 figures, 10 tables. Significant revision following referee's comments. Accepted for publication in MNRAS
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摘要：

本文重新分析了II-P型超新星2006 my、2006 ov和2004 et爆炸前的观测结果。在超新星2006 my和2006 ov的情况下，我们认为，公布的候选祖先是不符合各自的超新星爆炸前的哈勃空间望远镜观测网站。因此，我们推导出这两颗超新星看不见的祖先的光度和质量上限，假设它们是红超巨星：2006 my（log L/Lsun = 4.51;质量<13 Msun）和2006 ov（log L/Lsun = 4.29;质量<10 Msun）。在超新星2004 et的情况下，我们表明，黄超巨星的祖先候选人，最初在加拿大法国夏威夷望远镜的图像，仍然是可见的爆炸后3年的观测从威廉赫歇尔望远镜。高分辨率哈勃太空望远镜和双子座（北）自适应光学后期图像显示，这个来源不是一个单一的黄色超巨星，而是被分解成至少三个不同的来源。我们报告发现的未解决的祖作为一个过剩的流量在爆炸前艾萨克牛顿望远镜i波段成像。考虑到超新星的后期贡献，我们使用已发表的光谱计算了爆炸前和爆炸后地面观测之间的差异。我们发现它的前身极有可能是一颗8 + 5/-1 Msun的K型晚期到M型晚期超巨星。在所有的情况下，我们得出结论，未来，高分辨率的观测超新星网站将需要确认这些结果。

英文摘要：

The pre-explosion observations of the type II-P supernovae 2006my, 2006ov and 2004et, are re-analysed. In the cases of supernovae 2006my and 2006ov we argue that the published candidate progenitors are not coincident with their respective supernova sites in pre-explosion Hubble Space Telescope observations. We therefore derive upper luminosity and mass limits for the unseen progenitors of both these supernovae, assuming they are red supergiants: 2006my (log L/Lsun = 4.51; mass < 13Msun) and 2006ov (log L/Lsun = 4.29; mass < 10Msun). In the case of supernova 2004et we show that the yellow-supergiant progenitor candidate, originally identified in Canada France Hawaii Telescope images, is still visible ~3 years post-explosion in observations from the William Herschel Telescope. High-resolution Hubble Space Telescope and Gemini (North) adaptive optics late-time imagery reveal that this source is not a single yellow supergiant star, but rather is resolved into at least three distinct sources. We report the discovery of the unresolved progenitor as an excess of flux in pre-explosion Isaac Newton Telescope i'-band imaging. Accounting for the late-time contribution of the supernova using published optical spectra, we calculate the progenitor photometry as the difference between the pre- and post-explosion, ground-based observations. We find the progenitor was most likely a late K to late M-type supergiant of 8 +5/-1 Msun. In all cases we conclude that future, high-resolution observations of the supernova sites will be required to confirm these results.

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