中心分子带内$0.7^\circ\times0.4^\circ$的CARMA 3 mm测量
The CARMA 3mm Survey of the Inner $0.7^\circ\times0.4^\circ$ of the Central Molecular Zone
摘要：
银河系中心的中央分子带（CMZ）迄今为止只在毫米波段用单碟望远镜完全测绘过，分辨率约为30 $^{\prime\prime}$（1.2 pc）。使用CARMA，我们映射了CMZ的最里面的0.25平方度的区域之间的-0 $.\kern-.25em ^{^\circ}$ 2 $ \leq l \leq $ 0 $.\kern-.25em ^{^\circ}$ 5和-0 $.\kern-.25em ^{^\circ}$ 2 $ \leq b \leq $ 0 $.\kern-.25em ^{^\circ}$ 2（90 $\times$ 50 pc）的空间和光谱分辨率$\sim$ 10 $^{\prime\prime}$（0.4 pc）和$\sim$ 2.5 km/s，分别。我们提供了一个3毫米连续谱源的目录以及SiO（J=2-1）、HCO $^{+}$（J=1 -0）、HCN（J= 1 - 0）、N $_{2}$ H $^{+}$（J=1-0）和CS（J=2-1）的谱线图像，速度覆盖范围VLSR= -200 ~200 km/s。为了恢复由干涉仪分辨出的大尺度结构，将连续减影谱线图像与来自Mopra 22米望远镜巡天的数据相结合，从而提供包含所有空间频率的地图，直到分辨率极限。发现I（HCN）/I（HCO $^{+}$）的积分强度比与6.4 keV Fe K $α$的强度存在反相关关系，而HCO $^{+}$追踪的气体速度色散与Fe K $α$的强度存在相关关系.强度比和速度色散模式与预期的变化一致，从低能宇宙射线与分子气体的相互作用。
英文摘要：
The Central Molecular Zone (CMZ) of the Galactic Center has to date only been fully mapped at mm wavelengths with singledish telescopes, with resolution about 30$^{\prime\prime}$ (1.2 pc). Using CARMA, we mapped the innermost 0.25 square degrees of the CMZ over the region between -0$.\kern-.25em ^{^\circ}$2$ \leq l \leq $0$.\kern-.25em ^{^\circ}$5 and -0$.\kern-.25em ^{^\circ}$2$ \leq b \leq $0$.\kern-.25em ^{^\circ}$2 (90$\times$50 pc) with spatial and spectral resolution of $\sim$10$^{\prime\prime}$ (0.4 pc) and $\sim$2.5 km/s, respectively. We provide a catalog of 3mm continuum sources as well as spectral line images of SiO(J=2-1), HCO$^{+}$(J=1-0), HCN(J=1-0), N$_{2}$H$^{+}$(J=1-0), and CS(J=2-1), with velocity coverage VLSR= -200 to 200 km/s. To recover the large scale structure resolved out by the interferometer, the continuum-subtracted spectral line images were combined with data from the Mopra 22-m telescope survey, thus providing maps containing all spatial frequencies down to the resolution limit. We find that integrated intensity ratio of I(HCN)/I(HCO$^{+}$) is anti-correlated with the intensity of the 6.4 keV Fe K$α$, which is excited either by high energy photons or low energy cosmic rays, and the gas velocity dispersion as traced by HCO$^{+}$ is correlated with Fe K$α$ intensity. The intensity ratio and velocity dispersion patterns are consistent with variation expected from the interaction of low energy cosmic rays with molecular gas.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
