用H.E.S.S表征银河系中心200秒差距内的VHE弥散辐射
Characterising the VHE diffuse emission in the central 200 parsecs of our Galaxy with H.E.S.S
摘要：
H.E.S.S.在银河系中心200 pc观测到的弥散甚高能（VHE，> 100 GeV）伽马射线发射。的发现，遵循致密物质分布在中央分子区（CMZ）的纵向距离约130 pc的银河系中心（GC），在那里的流量迅速减少。最近的敏感性高血压。分析显示，宇宙射线（CR）密度分布随着到中心的距离而下降，使数据与GC的稳定宇宙PeVatron兼容。在本文中，我们扩展这种分析，以获得第一次详细的表征与物质的相关性，并寻找额外的功能和个人的伽玛射线源在内部200 pc。利用250个小时的高血压。数据和改进的分析技术，我们进行了详细的形态学研究的扩散VHE发射观察到的GC脊和重建其总光谱。我们发现，与致密物质相关的发射覆盖了整个CMZ，其通量约为总漫射发射通量的一半。我们还检测到一些发射在较高的纬度可能产生的强子碰撞的CR在较低密度的区域的GC星际介质。我们检测到一个额外的发射组件集中在GC和延伸超过约15 pc，这是一致的存在一个强大的CR密度梯度，并确认存在一个CR加速器在我们的银河系的中心。我们发现，全脊漫发射的光谱是兼容的与以前来自中心区域，这表明一个单一的人口的粒子填充整个CMZ。最后，我们报告了在GC射电弧附近发现的VHE伽马射线源，并认为它是由脉冲星风星云候选者G0.13-0.11产生的。
英文摘要：
The diffuse very high-energy (VHE, > 100 GeV) gamma-ray emission observed in the central 200 pc of the Milky Way by H.E.S.S. was found to follow the dense matter distribution in the Central Molecular Zone (CMZ) up to a longitudinal distance of about 130 pc to the Galactic Centre (GC), where the flux rapidly decreases. Recent sensitive H.E.S.S. analysis revealed that the cosmic-ray (CR) density profile drops with the distance to the centre, making data compatible with a steady cosmic PeVatron at the GC. In this paper, we extend this analysis to obtain for the first time a detailed characterisation of the correlation with matter and to search for additional features and individual gamma-ray sources in the inner 200 pc. Taking advantage of 250 hours of H.E.S.S. data and improved analysis techniques we perform a detailed morphology study of the diffuse VHE emission observed from the GC ridge and reconstruct its total spectrum. We show that the emission correlated with dense matter covers the full CMZ and that its flux is about half the total diffuse emission flux. We also detect some emission at higher latitude likely produced by hadronic collisions of CRs in less dense regions of the GC interstellar medium. We detect an additional emission component centred on the GC and extending over about 15 pc that is consistent with the existence of a strong CR density gradient and confirms the presence of a CR accelerator at the very centre of our Galaxy. We show that the spectrum of the full ridge diffuse emission is compatible with the one previously derived from the central regions, suggesting that a single population of particles fills the entire CMZ. Finally, we report the discovery of a VHE gamma-ray source near the GC radio arc and argue that it is produced by the pulsar wind nebula candidate G0.13-0.11.
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