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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >Suzaku observation of the unidentified very high energy gamma-ray source HESS J1702-420
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Suzaku observation of the unidentified very high energy gamma-ray source HESS J1702-420

机译：朱雀对未知高能伽玛射线源HESS J1702-420的观测

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A deep X-ray observation of the unidentified very high energy (VHE) gamma-ray source HESS J1702-420, for the first time, was carried out by Suzaku. No bright sources were detected in the XIS field of view (FOV), except for two faint point-like sources. The two sources, however, are considered not to be related to HESS J1702-420, because their fluxes in the 2-10 keV band (～10 ~(-14) erg s ~(-1) cm ~(-2)) are ～3 orders of magnitude smaller than the VHE gamma-ray flux in the 1-10TeV band (FTeV = 3.1 × 10 ~(-11) erg s ~(-1) cm ~(-2)). We compared the energy spectrum of diffuse emission, extracted from the entire XIS FOV with those from nearby observations. If we consider the systematic error of background subtraction, no significant diffuse emission was detected with an upper limit of F _X < 2.7 × 10 ~(-12) erg s ~(-1) cm ~(-2) in the 2-10 keV band for an assumed power-law spectrum of Γ = 2.1 and a source size same as that in the VHE band. The upper limit of the X-ray flux is twelve-times as small as the VHE gammaray flux. The large flux ratio (F _(TeV)=F _X) indicates that HESS J1702-420 is another example of a "dark" particle accelerator. If we use a simple one-zone leptonic model, in which VHE gamma-rays are produced through inverse Compton scattering of the cosmic microwave background and interstellar far-infrared emission, and the X-rays via the synchrotron mechanism, an upper limit of the magnetic field (1.7μG) is obtained from the flux ratio. Because the magnetic field is weaker than the typical value in the galactic plane (3-10μG), the simple one-zone model may not work for HESS J1702-420 and a significant fraction of the VHE gamma-rays may originate from protons.
机译：Suzaku首次对未识别的极高能量（VHE）γ射线源HESS J1702-420进行了深X射线观察。除了两个微弱的点状光源外，在XIS视场（FOV）中未检测到任何亮光源。但是，这两个源被认为与HESS J1702-420无关，因为它们在2-10 keV频带（〜10〜（-14）erg s〜（-1）cm〜（-2））中的通量。比1-10TeV波段的VHE伽马射线通量小3个数量级（FTeV = 3.1×10〜（-11）erg s〜（-1）cm〜（-2））。我们比较了从整个XIS FOV中提取的散射发射的能谱与从附近观测中获得的能谱。如果考虑背景扣除的系统误差，则在2-10中未检测到明显的漫射发射，其上限为F _X <2.7×10〜（-12）erg s〜（-1）cm〜（-2）假设Γ= 2.1的幂律谱的keV频带，并且源大小与VHE频带相同。 X射线通量的上限是VHEγ射线通量的十二倍。大通量比（F _（TeV）= F _X）表示HESS J1702-420是“深色”粒子促进剂的另一个示例。如果我们使用一个简单的单区轻子模型，其中VHE伽马射线是通过宇宙微波背景和星际远红外发射的逆康普顿散射产生的，而X射线是通过同步加速器机理产生的，从通量比获得磁场（1.7μG）。由于磁场弱于银河平面中的典型值（3-10μG），因此简单的单区模型可能不适用于HESS J1702-420，并且很大一部分VHE伽马射线可能来自质子。

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