M101超新星遗迹的物理结构和性质
Physical Structure and Nature of Supernova Remnants in M101
摘要：
巨大旋涡星系M101中的超新星遗迹（SNR）候选者先前已经从地面H-α和[SII]图像中识别出来。我们已经使用档案哈勃太空望远镜（HST）的H-α和宽带图像，以及恒星测光的55 SNR候选人，以检查他们的物理结构，星际环境，和潜在的恒星星族。我们还获得了高色散阶梯光谱搜索冲击高速气体在18 SNR候选人，并确定了X射线对应SNR候选人使用的数据从钱德拉X射线天文台的档案观测。这55个SNR候选者中有21个具有X射线对应物，尽管其中一个是已知的超亮X射线源。多波长信息已被用来评估每个SNR候选的性质。我们发现，在这个有限的样本中，~16%可能是Ia型SNe的残余，~45%是核心塌陷SNe的残余。此外，约36%是大的候选者，我们建议是超级气泡或OB/HII复合物。现有的无线电观测不够灵敏，无法检测到这些SNR候选者的非热发射。一些射电源与X射线源重合，但它们与M101中的巨大HII区域或背景星系有关。存档的HST H-alpha图像没有覆盖整个星系，因此无法对M101进行完整的研究。此外，HST [SII]图像的缺乏排除了对地面观测无法识别的小SNR候选者的搜索。这样的高分辨率图像是需要的，以获得一个完整的人口普查的SNRs在M101的分布，人口和该星系的SNe率的全面调查。
英文摘要：
Supernova remnant (SNR) candidates in the giant spiral galaxy M101 have been previously identified from ground-based H-alpha and [SII] images. We have used archival Hubble Space Telescope (HST) H-alpha and broad-band images as well as stellar photometry of 55 SNR candidates to examine their physical structure, interstellar environment, and underlying stellar population. We have also obtained high-dispersion echelle spectra to search for shocked high-velocity gas in 18 SNR candidates, and identified X-ray counterparts to SNR candidates using data from archival observations made by the Chandra X-ray Observatory. Twenty-one of these 55 SNR candidates studied have X-ray counterparts, although one of them is a known ultra-luminous X-ray source. The multi-wavelength information has been used to assess the nature of each SNR candidate. We find that within this limited sample, ~16% are likely remnants of Type Ia SNe and ~45% are remnants of core-collapse SNe. In addition, about ~36% are large candidates which we suggest are either superbubbles or OB/HII complexes. Existing radio observations are not sensitive enough to detect the non-thermal emission from these SNR candidates. Several radio sources are coincident with X-ray sources, but they are associated with either giant HII regions in M101 or background galaxies. The archival HST H-alpha images do not cover the entire galaxy and thus prevents a complete study of M101. Furthermore, the lack of HST [SII] images precludes searches for small SNR candidates which could not be identified by ground-based observations. Such high-resolution images are needed in order to obtain a complete census of SNRs in M101 for a comprehensive investigation of the distribution, population, and rates of SNe in this galaxy.
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