Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?
Can the Fe K-alpha Line Reliably Predict Supernova Remnant Progenitors?
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DOI：
10.3847/1538-4357/ac2305
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发表时间：
2021-09
期刊：
影响因子：
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通讯作者：
Jared E Siegel;V. Dwarkadas;K. Frank;D. Burrows
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作者：
Jared E Siegel;V. Dwarkadas;K. Frank;D. Burrows
Fe Kα线的质心能量已被用来鉴别超新星遗迹（SNRs）的祖先。这些研究通常考虑从整个残骸的光谱中得到的质心能量。在这里，我们使用XMM-牛顿数据来研究6个SNR中的Fe Kα质心：3C 397，N132 D，W 49 B，DEM L71，1 E 0102.2-7219和Kes 73。在Kes 73和1 E 0102.2-7219中，我们没有检测到任何Fe Kα发射。我们报告了在SNR DEM L71中首次探测到Fe Kα发射的尝试，其质心能量与其Ia型命名一致。在剩余的残骸中，空间和光谱灵敏度足以调查Fe Kα质心的空间变化。我们在N132 D和W 49 B中发现，不同区域的质心与从整体光谱中得出的质心一致，尽管不一定与通过其他方法确定的残留物类型一致。然而，在SNR 3C 397中，我们发现在高达100 eV的质心中的统计学显著变化，与残余物周围的密度结构中的变化一致。这些变化跨越了质心能量之间的中间空间，表示核心坍缩（CC）和Ia型残留物。将分界线向下移动50 eV可以将所有质心放置在CC区域中，但与通过其他方法获得的残余物类型相矛盾。我们的研究结果表明，必须谨慎使用时，采用的Fe Kα质心的整个残留物作为唯一的诊断分型残留物。
The centroid energy of the Fe Kα line has been used to identify the progenitors of supernova remnants (SNRs). These investigations generally considered the energy of the centroid derived from the spectrum of the entire remnant. Here we use XMM-Newton data to investigate the Fe Kα centroid in 6 SNRs: 3C 397, N132D, W49B, DEM L71, 1E 0102.2-7219, and Kes 73. In Kes 73 and 1E 0102.2-7219, we fail to detect any Fe Kα emission. We report a tentative first detection of Fe Kα emission in SNR DEM L71 with a centroid energy consistent with its Type Ia designation. In the remaining remnants, the spatial and spectral sensitivity is sufficient to investigate spatial variations of the Fe Kα centroid. We find in N132D and W49B that the centroids in different regions are consistent with those derived from the overall spectrum, although not necessarily with the remnant type identified via other means. However, in SNR 3C 397, we find statistically significant variation in the centroid of up to 100 eV, aligning with the variation in the density structure around the remnant. These variations span the intermediate space between centroid energies signifying core-collapse (CC) and Type Ia remnants. Shifting the dividing line downwards by 50 eV can place all the centroids in the CC region, but contradicts the remnant type obtained via other means. Our results show that caution must be used when employing the Fe Kα centroid of the entire remnant as the sole diagnostic for typing a remnant.