Arp 220中[ CI ] $^{3}P_{1}$ - $^{3}P_{0}$和$^{12}$ CO（1-0）之间的空间分辨关系
Spatially-resolved relation between [CI] $^{3}P_{1}$-$^{3}P_{0}$ and $^{12}$CO (1-0) in Arp 220
摘要：
我们介绍$\sim$ 0.“3（114 pc）分辨率的[CI] $^{3}P_{1}$ - $^{3}P_{0}$（以下简称[CI]（1-0））和$^{12}$ CO（1-0）的地图，使用阿塔卡马大型毫米/亚毫米阵列朝向Arp 220获得。[Cl]（1-0）排放的总体分布与CO（1-0）一致。对于未分辨的ULIRG样品，[CI]（1-0）和CO（1-0）的光度符合经验线性关系，而对于空间分辨的数据，我们发现[CI]（1-0）和CO（1-0）之间存在次线性关系。我们测量了Arp 220恒星形成环境中每个像元的[CI]（1-0）/CO（1-0）光度比，并研究了它对CO（3-2）/CO（1-0）比值（$R_{\rm CO}$）的依赖性。平均而言，[CI]（1-0）/CO（1-0）光度比在达到$R_{\rm CO} \simeq 1$之前几乎是恒定的，然后随着$R_{\rm CO}$而增加。根据辐射传输分析，在[CI]（1-0）/CO（1 -0）光度比和$R_{\rm CO} > 1$高的区域需要高的CI/CO丰度比，这表明CI/CO丰度比在Arp 220的$\sim$ 100 pc尺度上变化。[CI]（1-0）/CO（1-0）光度比取决于多种因素，可能无法直接解释。我们还发现了由[CI]（1-0）跟踪的西核的高速分量，可能与分子外流有关。[CI]（1-0）/CO（1-0）的光度比为0.87 $\pm$ 0.28，比Arp 220的平均比值高出4倍。虽然[CI]（1-0）和CO（1-0）的发射可能是不同组分的示踪物，但我们认为高的谱线比可能是因为基于我们的辐射传递分析的Cl/CO丰度比升高。宇宙射线的照射、激波加热和强辐射场可能导致流出物中的富CI和贫CO气相。
英文摘要：
We present $\sim$0."3 (114 pc) resolution maps of [CI] $^{3}P_{1}$-$^{3}P_{0}$ (hereafter [CI] (1-0)) and $^{12}$CO (1-0) obtained toward Arp 220 with the Atacama Large Millimeter/submillimeter Array. The overall distribution of the [CI] (1-0) emission is consistent with the CO (1-0). While the [CI] (1-0) and CO (1-0) luminosities of the system follow the empirical linear relation for the unresolved ULIRG sample, we find a sublinear relation between [CI] (1-0) and CO (1-0) using the spatially-resolved data. We measure the [CI] (1-0)/CO (1-0) luminosity ratio per pixel in star-forming environments of Arp 220 and investigate its dependence on the CO (3-2)/CO (1-0) ratio ($R_{\rm CO}$). On average, the [CI] (1-0)/CO (1-0) luminosity ratio is almost constant up to $R_{\rm CO} \simeq 1$ and then increases with $R_{\rm CO}$. According to the radiative transfer analysis, a high CI/CO abundance ratio is required in regions with high [CI] (1-0)/CO (1-0) luminosity ratios and $R_{\rm CO} > 1$, suggesting that the CI/CO abundance ratio varies at $\sim$100 pc scale in Arp 220. The [CI] (1-0)/CO (1-0) luminosity ratio depends on multiple factors and may not be straightforward to interpret. We also find the high-velocity components traced by [CI] (1-0) in the western nucleus, likely associated with the molecular outflow. The [CI] (1-0)/CO (1-0) luminosity ratio in the putative outflow is 0.87 $\pm$ 0.28, which is four times higher than the average ratio of Arp 220. While there is a possibility that the [CI] (1-0) and CO (1-0) emission traces different components, we suggest that the high line ratios are likely because of elevated CI/CO abundance ratios based on our radiative transfer analysis. A CI-rich and CO-poor gas phase in outflows could be caused by the irradiation of the cosmic rays, the shock heating, and the intense radiation field.
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