将ISM连接到TeV PWNe和PWNe候选
Connecting the ISM to TeV PWNe and PWNe candidates
摘要：
利用Mopra分子谱线7 mm观测数据[CS（1-0），SiO（1-0，v=0）]，Nanten CO（1 - 0）数据和SGPS/GASS HI巡天，研究了7个TeV γ射线源的星际介质（ISM），这些γ射线源被认为是脉冲星风星云（PWNe）。我们已经发现了几个密集的分子云共同定位到这些TeV的伽马射线源，这使我们能够搜索宇宙射线（CR）来自祖SNR或潜在的，从PWNe。我们特别发现了HESS J1809-193的SiO（1-0，v=0）发射，突出了相邻超新星遗迹SNR G011.0-0.0与d $\sim$ 3.7 kpc分子云之间可能的相互作用。使用形态学特征，以及我们的柱密度与X射线测量获得的柱密度的比较研究，我们声明SNR G292.2-00.5的距离d $\sim$为8.6 - 9.7 kpc，PSR J1418-6058的距离d $\sim$为3.5 - 5.6 kpc，HESS J1303-631的新SNR候选物的距离d $\sim$为1.5 kpc。从我们的质量和密度估计选定的分子云，我们讨论的签名强子/轻子组件PWNe和他们的祖先信噪比。有趣的是，在d $\sim$ 5 kpc处与HESS J1026-582重叠的分子气体可能支持强子起源。然而，我们发现，这种情况下需要一个未被发现的宇宙射线加速器位于d $\lt$ 10 pc的分子云。对于HESS J1809-193，逃逸SNR G011.0-0.0的宇宙射线可能对TeV γ射线发射有贡献。最后，从最多20%的脉冲星自旋下降功率可以转换为CR的假设，我们发现，在所研究的PWNe，只有那些从PSR J1809-1917可能有助于TeV的排放。
英文摘要：
We investigate the interstellar medium (ISM) towards seven TeV gamma-ray sources thought to be pulsar wind nebulae (PWNe) using Mopra molecular line observations at 7mm [CS(1-0), SiO(1-0,v=0)], Nanten CO(1-0) data and the SGPS/GASS HI survey. We have discovered several dense molecular clouds co-located to these TeV gamma-ray sources , which allows us to search for cosmic-rays (CRs) coming from progenitor SNRs or, potentially, from PWNe. We notably found SiO(1-0,v=0) emission towards HESS J1809-193, highlighting possible interaction between the adjacent supernova remnant SNR G011.0-0.0 and the molecular cloud at d $\sim$ 3.7 kpc. Using morphological features, and comparative studies of our column densities with those obtained from X-ray measurements, we claim a distance d $\sim$ 8.6 - 9.7 kpc for SNR G292.2-00.5, d $\sim$ 3.5 - 5.6 kpc for PSR J1418-6058 and d $\sim$ 1.5 kpc for the new SNR candidate found towards HESS J1303-631. From our mass and density estimates of selected molecular clouds, we discuss signatures of hadronic/leptonic components from PWNe and their progenitor SNRs. Interestingly, the molecular gas, which overlaps HESS J1026-582 at d $\sim$ 5 kpc, may support a hadronic origin. We find however that this scenario requires an undetected cosmic-ray accelerator to be located at d $\lt$ 10 pc from the molecular cloud. For HESS J1809-193, the cosmic-rays which have escaped SNR G011.0-0.0 could contribute to the TeV gamma-ray emission. Finally, from the hypothesis that at most 20% the pulsar spin down power could be converted into CRs, we find that, among the studied PWNe, only those from PSR J1809-1917 could potentially contribute to the TeV emission.
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