心脏Milky Way：研究中心分子区的分子气体和gamma-ray形态
The Milky Way Heart: Investigating molecular gas and gamma-ray morphologies in the Central Molecular Zone
摘要：
自2006年HESS合作组在银河系中央分子区（CMZ）发现了广泛分布的甚高能量（VHE; >0.1 TeV）伽马射线以来，这种发射与CS（1-0）分子线发射的积分强度的相关性推断了伽马射线的强子起源。在这里，我们描述了我们的调查开始到这种相关性的强度利用新的多线毫米波数据从Mopra CMZ和HOP调查和多波长GBT无线电连续观测对CMZ和比较这些详细的扩散TeV伽马射线发射从HESS。这些新数据的好处是，它们允许我们使用大量（>10）分子种类同时观察和分析相关性，其中一些包含它们的同位素对。同位素对的使用特别强大，因为它允许分析许多不同分子种类的光学深度，从而研究在一系列不同物理条件下相关性的性质。在这里，我们开始比较的综合线发射和连续射电发射与弥漫的伽玛射线发射，并通过使用同位素对，如HCN/H $^{13}$ CN，获得整个CMZ的光学深度对应的区域的强和弱的伽玛射线发射。我们发现，无线电连续更好地匹配伽马射线发射的峰值，这对应于更紧凑-相比，相对粗糙的分辨率的伽马射线图像-CMZ中的源。利用同位素对，我们发现在CMZ内的所有位置和速度的光学深度约为2- 4。这与CS（1- 0）线的发现相似，并且会低估CMZ的质量，这可能解释了为什么分子线发射峰似乎偏离伽马射线峰。
英文摘要：
Since the discovery of a broad distribution of very high energy (VHE; >0.1 TeV) gamma-rays in the Central Molecular Zone (CMZ) of the Galaxy in 2006 by the HESS collaboration, the correlation of this emission with the integrated intensity of the CS(1-0) molecular line emission has inferred a hadronic origin for the gamma-rays. Here we describe the beginning of our investigation into the strength of this correlation utilising new multi-line millimeter data from the Mopra CMZ and HOP surveys and multi-wavelength GBT radio continuum observations towards the CMZ and compare these in detail with the diffuse TeV gamma-ray emission from HESS. The benefit of these new data is that they allow us to simultaneously observe and analyse correlations using a large number (>10) of molecular species, some of which contain their isotopologue pairs. The use of isotopologue pairs is especially powerful, since it allows one to analyse the optical depth of a number of different molecular species, thus investigating the nature of the correlation over a range of different physical conditions. Here we begin by comparing the integrated line emission and continuum radio emission with the diffuse gamma-ray emission, and, by using isotopologue pairs such as HCN/H$^{13}$CN, obtain optical depths throughout the CMZ corresponding to regions of both strong and weak gamma-ray emission. We find that the radio continuum better matches the peak of the gamma-ray emission, which corresponds to the more compact -- compared to the relatively coarse resolution of the gamma-ray images -- sources in the CMZ. Using the isotopologue pairs, we find that the optical depth at all positions and velocities within the CMZ are about 2--4. This is similar to that found for the CS(1--0) line and would underestimate the mass of the CMZ, potentially explaining why molecular line emission peaks appear offset from the gamma-ray peaks.
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