Detection of X-Ray Emission from the Unidentified TeV Gamma-Ray Source TeV J2032+4130
Detection of X-Ray Emission from the Unidentified TeV Gamma-Ray Source TeV J2032+4130
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DOI：
10.1093/pasj/63.sp3.s873
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发表时间：
2011-11
影响因子：
2.3
通讯作者：
H. Murakami;S. Kitamoto;A. Kawachi;T. Nakamori
中科院分区：
文献类型：
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作者：
H. Murakami;S. Kitamoto;A. Kawachi;T. Nakamori
我们用铃鹿观测了fi第一个统一的fiED TeVγ源TeVJ2032+4130。由于Suzaku对利用X射线发射检测diff具有很高的灵敏度，我们在TeV发射区发现了两个小结构。其中一个与费米-伽马射线太空望远镜发现的γ-ray脉冲星PSRJ2032+4127重合。通过减去由钱德拉数据估计的点源的贡献，我们得到了利用X射线光谱的diff。X射线能谱可用光子指数为∼2的幂定律模型和2×10−13erg S−1 cm−2的X射线UX重现。γ-rayflUX与X-rayflUX的比率约为10。如果TeVγ射线的起源是高能电子对微波背景的逆康普顿散射，则该比率对应于fi1微米的∼磁场强度。然而，X射线发射的尺寸比TeV发射的小，这表明电子扫描的能量损失解释了γ-rayflUX的大比例，合理的磁fi场强为几微克。关键词：粒子-X射线的加速：个体(TeV J2032+4130)-X射线：ISM-脉冲星：个体(PSRJ2032+4127)1.介绍大气切伦科夫望远镜的立体技术提高了探测TeVγ射线的角分辨率，从而增加了TeVγ-射线源的数量。一些新的TeV天体在其他波长上没有对应的天体，它们被称为Unidentified TeVγ-ray天体。这些天体为研究高能宇宙射线的起源提供了关键信息。对这些天体的多波长观测对于阐明它们的发射机制和成功地识别fi是非常重要的。TeV J2032+4130是Hegra发现的第一个唯一的fified TeVγ光源。2002年)。TeV排放呈现出明显的fiCan延伸，半径为6。
AbstractWe observed the first unidentified TeV γ-ray source TeV J2032+4130 with Suzaku. Owing to Suzaku’shigh sensitivity for detection of diffuse X-ray emission, we found two small structures in the TeV emittingregion. One of them is coincident with a γ-ray pulsar PSR J2032+4127, which was discovered by the FermiGamma-ray Space Telescope. By subtracting contribution of point sources estimated by Chandra data,we obtained diffuse X-ray spectrum. The X-ray spectrum can be reproduced by a power-law model with aphoton index of ∼ 2, and an X-ray flux of 2×10 −13 erg s −1 cm −2 . The ratio of the γ-ray flux to the X-rayflux is about 10. If the origin of the TeV γ-ray is inverse Compton scattering of microwave backgroundby high energy electrons, the ratio corresponds to the magnetic field strength of ∼ 1 µG. However, thesmaller size of the X-ray emission than that of the TeV emission suggests that energy loss of the electronscan explain the large ratio of the γ-ray flux with a reasonable magnetic field strength of a few µG.Key words: acceleration of particles — X-rays: individual (TeV J2032+4130) — X-rays: ISM —pulsars: individual (PSR J2032+4127)1. IntroductionThe stereoscopic technique of atmospheric Cerenkovtelescopes improved the angular resolution for detectingTeV γ-rays and thus increased the number of TeV γ-raysources. Some of new TeV objects have no counterparts atother wavelengths and are called unidentified TeV γ-rayobjects. These objects provide key information in the in-vestigationofthe originofhigh-energycosmicrays. Multi-wavelength observations of these objects are very impor-tant in elucidating the emission mechanism and successfulidentification of them.TeV J2032+4130 was the first unidentified TeV γ-raysource discovered by HEGRA (Aharonian et al. 2002).The TeV emission exhibits a significant extension witha radius of 6.