DISCRIMINATING THE PROGENITOR TYPE OF SUPERNOVA REMNANTS WITH IRON K-SHELL EMISSION
DISCRIMINATING THE PROGENITOR TYPE OF SUPERNOVA REMNANTS WITH IRON K-SHELL EMISSION
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DOI：
10.1088/2041-8205/785/2/l27
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发表时间：
2014-03
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通讯作者：
H. Yamaguchi;C. Badenes;R. Petre;T. Nakano;D. Castro;T. Enoto;J. Hiraga;J. Hughes;Y. Maeda;M. Nobukawa;S. Safi-Harb;P. Slane;Randall K. Smith;H. Uchida
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作者：
H. Yamaguchi;C. Badenes;R. Petre;T. Nakano;D. Castro;T. Enoto;J. Hiraga;J. Hughes;Y. Maeda;M. Nobukawa;S. Safi-Harb;P. Slane;Randall K. Smith;H. Uchida
超新星遗迹（SNRs）保留了关于其母爆炸和其祖先留下的星周物质的关键信息。然而，超新星喷出物和周围介质之间相互作用的复杂性往往模糊了这一信息，并且对于经过充分研究的遗迹的基本祖先类型（Ia或核心塌陷）仍然不确定并不罕见。在这里，我们提出了一个强大的新的观测诊断，以区分祖细胞类型和限制周围介质密度的信噪比仅使用铁K壳层X射线发射。我们分析了朱雀星现存的信噪比观测数据，并从23个年轻或中年的遗迹中检测到Fe Kα发射，包括5个首次检测到的遗迹（IC 443，G292.0+1.8，G337.2-0.7，N49和N63 A）。Fe Kα质心清楚地分离了祖先类型，Ia型残留物中富含Fe的喷出物比核心塌陷SNR中的电离程度要低得多。在每一个祖先群中，Fe Kα的光度和质心都有很好的相关性，更明亮的天体具有更高的电离Fe。我们的研究结果表明，爆炸类型和周围的介质密度之间有很强的联系，并建议Ia型超新星的祖先没有实质性地改变其周围的半径高达几个秒差距。我们还检测到的K壳层辐射复合连续的铁在W 49 B和IC 443，这意味着在这些核心崩溃残留物的早期演化阶段的强烈的拱星相互作用。
Supernova remnants (SNRs) retain crucial information about both their parent explosion and circumstellar material left behind by their progenitor. However, the complexity of the interaction between supernova ejecta and ambient medium often blurs this information, and it is not uncommon for the basic progenitor type (Ia or core-collapse) of well-studied remnants to remain uncertain. Here we present a powerful new observational diagnostic to discriminate between progenitor types and constrain the ambient medium density of SNRs using solely Fe K-shell X-ray emission. We analyze all extant Suzaku observations of SNRs and detect Fe Kα emission from 23 young or middle-aged remnants, including five first detections (IC 443, G292.0+1.8, G337.2–0.7, N49, and N63A). The Fe Kα centroids clearly separate progenitor types, with the Fe-rich ejecta in Type Ia remnants being significantly less ionized than in core-collapse SNRs. Within each progenitor group, the Fe Kα luminosity and centroid are well correlated, with more luminous objects having more highly ionized Fe. Our results indicate that there is a strong connection between explosion type and ambient medium density, and suggest that Type Ia supernova progenitors do not substantially modify their surroundings at radii of up to several parsecs. We also detect a K-shell radiative recombination continuum of Fe in W49B and IC 443, implying a strong circumstellar interaction in the early evolutionary phases of these core-collapse remnants.