G0 .9+0.1中PWN非热发射的空间分辨X射线光谱学和建模
Spatially resolved X-ray spectroscopy and modeling of the nonthermal emission of the PWN in G0.9+0.1
摘要：
我们对超新星遗迹G0.9+0.1中的脉冲星风星云（PWN）进行了空间分辨光谱X射线研究。此外，我们模拟了它的非热发射在X射线和非常高的能量（VHE，E > 100 GeV）的伽马射线制度。使用Chandra ACIS-S3数据，我们通过计算硬度比来研究G0.9+0.1光谱特性的东西依赖性。我们分析了EPIC-MOS和EPIC-pn数据的两个轴上观测的XMM-牛顿望远镜和提取光谱的四个环形区域，集中在最亮的发射源的区域。一个径向对称轻子模型，以再现所观察到的X射线发射的内部部分的PWN。使用从X射线分析获得的优化的模型参数值，然后我们将建模的逆康普顿（IC）辐射与已公布的H.E.S.S.伽马射线数据四个环带内的光谱指数随到脉冲星距离的增加而增加，而表面亮度则下降。利用所采用的模型，我们能够再现X射线谱的特征。然而，VHE伽马辐射的模型结果与H.E.S.S.数据
英文摘要：
We performed a spatially resolved spectral X-ray study of the pulsar wind nebula (PWN) in the supernova remnant G0.9+0.1. Furthermore we modeled its nonthermal emission in the X-ray and very high energy (VHE, E > 100 GeV) gamma-ray regime. Using Chandra ACIS-S3 data, we investigated the east-west dependence of the spectral properties of G0.9+0.1 by calculating hardness ratios. We analyzed the EPIC-MOS and EPIC-pn data of two on-axis observations of the XMM-Newton telescope and extracted spectra of four annulus-shaped regions, centered on the region of brightest emission of the source. A radially symmetric leptonic model was applied in order to reproduce the observed X-ray emission of the inner part of the PWN. Using the optimized model parameter values obtained from the X-ray analysis, we then compared the modeled inverse Compton (IC) radiation with the published H.E.S.S. gamma-ray data. The spectral index within the four annuli increases with growing distance to the pulsar, whereas the surface brightness drops. With the adopted model we are able to reproduce the characteristics of the X-ray spectra. The model results for the VHE gamma radiation, however, strongly deviate from the H.E.S.S. data.
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