Infrared and X-ray study of the Galactic SNR G15.9+0.2
Infrared and X-ray study of the Galactic SNR G15.9+0.2
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DOI：
10.1093/mnras/sty1596
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发表时间：
2018-06
影响因子：
4.8
通讯作者：
M. Sasaki;Minja M Mäkelä;D. Klochkov;A. Santangelo;V. Suleimanov
中科院分区：
文献类型：
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作者：
M. Sasaki;Minja M Mäkelä;D. Klochkov;A. Santangelo;V. Suleimanov
G15.9+0.2是一个银河壳型超新星遗迹（SNR），它是在射电中被发现的，并已在钱德拉的X射线观测中得到证实。探测到一个X射线点源CXOUJ 181852.0 -150213，并认为它是一颗伴生的中子星星。在最近的一项研究中，我们已经证实了源是一个中心致密天体（CCO）。我们已经研究了SNR使用高分辨率的X射线数据与钱德拉红外（IR）数据相结合，以了解其发射，并得出其物理参数。这也将有助于约束，例如，CCO的时代及其诞生的环境。使用新的钱德拉数据的X射线发射的光谱分析和红外数据的比较表明，SNR是相对年轻的几千年的年龄，它的发射是由受冲击的星际介质（ISM）的。然而，对明亮的东方壳层光谱的分析表明，有一个额外的发射成分，{\alpha}元素和Fe的丰度增加，这表明喷出物发射。多波长发射与在具有密度梯度的ISM中扩展的SNR G15.9+0.2一致，同时还存在位于SNR前面的较冷的材料，其在较软的频带中吸收其热X射线发射。
G15.9+0.2 is a Galactic shell-type supernova remnant (SNR), which was detected in radio and has been confirmed in X-rays based on Chandra observations. An X-ray point source CXOUJ181852.0-150213 has been detected and suggested to be an associated neutron star. In a recent study, we have confirmed the source to be a central compact object (CCO). We have studied the SNR using high-resolution X-ray data taken with Chandra in combination with infrared (IR) data in order to understand its emission and to derive its physical parameters. This will also help to constrain, e.g., the age of the CCO and the environment in which it was born. The spectral analysis of the X-ray emission using the new Chandra data and the comparison to the IR data have shown that the SNR is relatively young with an age of a few thousand years and that its emission is dominated by that of shocked interstellar medium (ISM). However, the analysis of the spectrum of the bright eastern shell shows that there is an additional emission component with enhanced abundances of {\alpha} elements and Fe, suggesting ejecta emission. The multi-wavelength emission is consistent with SNR G15.9+0.2 expanding in an ISM with a density gradient, while there is also colder material located in front of the SNR, which absorbs its thermal X-ray emission in the softer bands.