The Nature of a Cosmic-Ray Accelerator, CTB 37 B, Observed with Suzaku and Chandra
The Nature of a Cosmic-Ray Accelerator, CTB 37 B, Observed with Suzaku and Chandra
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DOI：
10.1093/pasj/61.sp1.s197
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发表时间：
2008-08
影响因子：
2.3
通讯作者：
R. Nakamura;A. Bamba;M. Ishida;H. Nakajima;R. Yamazaki;Y. Terada;G. Puhlhofer;S. Wagner
中科院分区：
文献类型：
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作者：
R. Nakamura;A. Bamba;M. Ishida;H. Nakajima;R. Yamazaki;Y. Terada;G. Puhlhofer;S. Wagner
我们报道了Suzaku和Chandra对年轻超新星遗迹CTB37B的观测，切伦科夫望远镜从这些遗迹探测到了TeV�射线。80K的Suzaku观测为我们提供了清晰的漫射图像和高质量的光谱。光谱分析表明，扩散发射由热组分和非热组分组成。温度、激前电子密度和年龄分别为0.9·0.2keV、0.4·0.1 cm�3和650+2500�300yr的NEI模型可表示热分量。这表明CTB-37B的爆炸发生在低密度空间。在CTB37B的南部区域发现了一个非热幂定律分量，它的光子指数为�1.5，并有很高的滚落能量(&15keV)，表明宇宙线加速是有效的。将这一X射线能谱与TeV�能谱进行比较，我们可以得出结论，TeV�的发射似乎是由多区逆康普顿散射或中性介子的衰变提供动力的。Chandra在壳层附近分辨出的点源可能与CTB37B有关，因为扩散热发射具有共同的氢柱密度。光谱和时间特征表明该源是一颗新的反常X射线脉冲星。
We report on Suzaku and Chandra observations of the young supernova remnant CTB 37 B, from which TeV � -rays were detected by the H.E.S.S. Cherenkov telescope. The 80 ks Suzaku observation provided us with a clear image of diffuse emission and high-quality spectra. The spectra revealed that the diffuse emission is comprised of thermal and non-thermal components. The thermal component can be represented by an NEI model with a temperature, a pre-shock electron density and an age of 0.9˙0.2 keV, 0.4˙0.1 cm � 3 , and 650 +2500 � 300 yr, respectively. This suggests that the explosion of CTB 37 B occurred in a low-density space. A non-thermal power-law component was found from the southern region of CTB 37 B. Its photon index of � 1.5 and a high roll-off energy (& 15 keV) indicate efficient cosmic-ray acceleration. A comparison of this X-ray spectrum with the TeV � -ray spectrum leads us to conclude that the TeV � -ray emission seems to be powered by either multi-zone Inverse Compton scattering or the decay of neutral pions. The point source resolved by Chandra near the shell is probably associated with CTB 37 B, because of the common hydrogen column density with the diffuse thermal emission. Spectral and temporal characteristics suggest that this source is a new anomalous X-ray pulsar.