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首页> 外文期刊>Astronomy and astrophysics >An X-ray study of the SNR G344.7-0.1 and the central object CXOU J170357.8-414302
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An X-ray study of the SNR G344.7-0.1 and the central object CXOU J170357.8-414302

机译：SNR G344.7-0.1和中心物体CXOU J170357.8-414302的X射线研究

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Aims. We report results of an X-ray study of the supernova remnant (SNR) G344.7-0.1 and the point-like X-ray source located at the geometrical center of the SNR radio structure. Methods. The morphology and spectral properties of the remnant and the central X-ray point-like source were studied using data from the XMM-Newton and Chandra satellites. Archival radio data and infrared Spitzer observations at 8 and 24?μm were used to compare and study its multi-band properties at different wavelengths. Results. The XMM-Newton and Chandra observations reveal that the overall X-ray emission of G344.7-0.1 is extended and correlates very well with regions of bright radio and infrared emission. The X-ray spectrum is dominated by prominent atomic emission lines. These characteristics suggest that the X-ray emission originated in a thin thermal plasma, whose radiation is represented well by a plane-parallel shock plasma model (PSHOCK). Our study favors the scenario in which G344.7-0.1 is a 6?×?103?year old SNR expanding in a medium with a high density gradient and is most likely encountering a molecular cloud on the western side. In addition, we report the discovery of a soft point-like X-ray source located at the geometrical center of the radio SNR structure. The object presents some characteristics of the so-called compact central objects (CCO). However, its neutral hydrogen absorption column (NH) is inconsistent with that of the SNR. Coincident with the position of the source, we found infrared and optical objects with typical early-K star characteristics. The X-ray source may be a foreground star or the CCO associated with the SNR. If this latter possibility were confirmed, the point-like source would be the farthest CCO detected so far and the eighth member of the new population of isolated and weakly magnetized neutron stars.
机译：目的我们报告了对超新星残余（SNR）G344.7-0.1和位于SNR无线电结构几何中心的点状X射线源进行X射线研究的结果。方法。使用来自XMM-Newton和Chandra卫星的数据研究了残留物和中心X射线点状源的形态和光谱特性。使用档案无线电数据和在8和24？m处的红外Spitzer观测值来比较和研究其在不同波长下的多波段特性。结果。 XMM-Newton和Chandra的观测表明，G344.7-0.1的总X射线发射得到扩展，并且与明亮的无线电和红外发射区域非常相关。 X射线光谱以突出的原子发射线为主。这些特征表明，X射线发射起源于薄的热等离子体，其辐射由平面平行冲击等离子体模型（PSHOCK）很好地表示。我们的研究偏向于这样一种场景，其中G344.7-0.1是一个6？×？103？年的SNR，它在具有高密度梯度的介质中扩展，并且最有可能在西侧遇到分子云。此外，我们报告了位于无线电SNR结构几何中心的类似软点X射线源的发现。该对象具有所谓的紧凑型中心对象（CCO）的某些特征。但是，其中性氢吸收柱（NH）与SNR不一致。与光源的位置相吻合，我们发现了具有典型早K星特征的红外和光学物体。 X射线源可以是前景星或与SNR相关联的CCO。如果证实了后者的可能性，则点状源将是迄今为止检测到的最远的CCO，并且是新的孤立和弱磁中子星群的第八个成员。

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