Supernova progenitors, their variability and the Type IIP Supernova ASASSN-16fq in M66
Supernova progenitors, their variability and the Type IIP Supernova ASASSN-16fq in M66
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DOI：
10.1093/mnras/stx291
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发表时间：
2016-08
影响因子：
4.8
通讯作者：
C. Kochanek;M. Fraser;S. Adams;T. Sukhbold;J. Prieto;T. Muller;G. Bock;J. Brown;S. Dong
中科院分区：
文献类型：
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作者：
C. Kochanek;M. Fraser;S. Adams;T. Sukhbold;J. Prieto;T. Muller;G. Bock;J. Brown;S. Dong
我们在哈勃太空望远镜的存档数据中发现了附近IIP型超新星ASASSN-16 fq（SN 2016 cok）的爆炸前对应物。该源似乎是几颗恒星的混合物，这妨碍了获得准确的测光。然而，通过对恒星温度和灭绝的合理假设，几乎可以肯定的是，这颗恒星的初始质量为M*<$17 M <$，并且很可能在M* = 8-12 M <$的质量范围内。一旦ASASSN-16 fq褪色，观察结果将不难准确确定祖先的属性。在8年的大双筒望远镜（LBT）数据中，没有发现明显的祖先变异，均方根极限约为0.03 mag.6附近的超新星（SN）的低水平变异的限制，SN 1987 A，SN 1993 J，SN 2008 cn，SN 2011 dh，SN 2013 ej和ASASSN-16 fq，只有SN 2011 dh的缓慢褪色的前身显示出明显的变异性证据。不包括SN 1987 A，在SN 1987 A之前的过去十年中，持续时间超过0.1年（半峰全宽）且亮度超过MR <-8等的爆发次数的90%置信限约为Nout = 1.3。我们持续的LBT监测计划将稳步改善对SN前祖先变异的限制，其幅度远低于SN调查所能达到的幅度。
We identify a pre-explosion counterpart to the nearby Type IIP supernova ASASSN-16fq (SN 2016cok) in archival Hubble Space Telescope data. The source appears to be a blend of several stars that prevents obtaining accurate photometry. However, with reasonable assumptions about the stellar temperature and extinction, the progenitor almost certainly had an initial mass M* ≲ 17 M⊙, and was most likely in the mass range of M* = 8–12 M⊙. Observations once ASASSN-16fq has faded will have no difficulty accurately determining the properties of the progenitor. In 8 yr of Large Binocular Telescope (LBT) data, no significant progenitor variability is detected to rms limits of roughly 0.03 mag. Of the six nearby supernova (SN) with constraints on the low-level variability, SN 1987A, SN 1993J, SN 2008cn, SN 2011dh, SN 2013ej and ASASSN-16fq, only the slowly fading progenitor of SN 2011dh showed clear evidence of variability. Excluding SN 1987A, the 90 per cent confidence limit implied by these sources on the number of outbursts over the last decade before the SN that last longer than 0.1 yr (full width at half-maximum) and are brighter than MR < −8 mag is approximately Nout ≲ 3. Our continuing LBT monitoring programme will steadily improve constraints on pre-SN progenitor variability at amplitudes far lower than achievable by SN surveys.