Discovery of Extended X-Ray Emission from an Unidentified TeV Source, HESS J1614$-$518, Using the Suzaku Satellite
Discovery of Extended X-Ray Emission from an Unidentified TeV Source, HESS J1614$-$518, Using the Suzaku Satellite
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DOI：
10.1093/pasj/60.sp1.s163
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发表时间：
2007-12
影响因子：
2.3
通讯作者：
H. Matsumoto;H. Uchiyama;M. Sawada;T. Tsuru;K. Koyama;H. Katagiri;R. Yamazaki;A. Bamba;K. Kohri;K. Mori;Yasunobu Uchiyama Kyoto University;Hiroshima University;Isasjaxa;L. University;M. University
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作者：
H. Matsumoto;H. Uchiyama;M. Sawada;T. Tsuru;K. Koyama;H. Katagiri;R. Yamazaki;A. Bamba;K. Kohri;K. Mori;Yasunobu Uchiyama Kyoto University;Hiroshima University;Isasjaxa;L. University;M. University
我们报告了HESS J1614-518的Suzaku结果，这是在使用H.E.S.S.望远镜进行的银河面调查中发现的最亮的扩展TeV伽玛射线源。我们在x射线成像光谱仪（XIS）的视场中发现了三个x射线天体，命名为Suzaku J1614-5141 (src A), Suzaku J1614-5152 （src B）和Suzaku J1614-5148 （src C）。Src A是位于HESS J1614-518峰值位置的扩展源，因此它可能与HESS J1614-518相对应。2-10 keV波段的x射线通量为5e-13 erg/s/cm^2，比TeV的通量小一个数量级。光子指数为1.7，这比在一些超新星残骸中发现的高能电子同步辐射的标准值要小。这些发现对一些模型提出了挑战，在这些模型中，TeV发射的起源是宇宙微波背景的逆康普顿散射，这种散射是由加速电子通过同步辐射发射x射线产生的。Src B在TeV波段图像中位于相对较暗的区域；但其氢柱密度与src a相同，因此src B也可能与HESS J1614-518存在物理关系。Src C是一颗前景晚B型恒星。我们还在HESS J1614-518附近发现了软扩展x射线发射。
We report the Suzaku results of HESS J1614-518, which is the brightest extended TeV gamma-ray source discovered in the Galactic plane survey conducted using the H.E.S.S. telescope. We discovered three X-ray objects in the field of view of the X-ray Imaging Spectrometer (XIS), which were designated as Suzaku J1614-5141 (src A), Suzaku J1614-5152 (src B), and Suzaku J1614-5148 (src C). Src A is an extended source located at the peak position of HESS J1614-518, and therefore it is a plausible counterpart to HESS J1614-518. The X-ray flux in the 2-10 keV band is 5e-13 erg/s/cm^2, which is an order of magnitude smaller than the TeV flux. The photon index is 1.7, which is smaller than the canonical value of synchrotron emissions from high-energy electrons found in some supernova remnants. These findings present a challenge to models in which the origin of the TeV emission is the inverse Compton scattering of the cosmic microwave background by accelerated electrons that emit X-rays via synchrotron emission. Src B is located at a relatively dim region in the TeV band image; however, its hydrogen column density is the same as that of src A. Therefore, src B may also be physically related to HESS J1614-518. Src C is a foreground late-type B star. We also discovered a soft extended X-ray emission near HESS J1614-518.