English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

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) obtainedtoward Arp 220 with the Atacama Large Millimeter/submillimeter Array. Theoverall 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 theempirical linear relation for the unresolved ULIRG sample, we find a sublinearrelation between [CI] (1-0) and CO (1-0) using the spatially-resolved data. Wemeasure the [CI] (1-0)/CO (1-0) luminosity ratio per pixel in star-formingenvironments 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 isalmost constant up to $R_{\rm CO} \simeq 1$ and then increases with $R_{\rmCO}$. According to the radiative transfer analysis, a high CI/CO abundanceratio is required in regions with high [CI] (1-0)/CO (1-0) luminosity ratiosand $R_{\rm CO} > 1$, 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 dependson multiple factors and may not be straightforward to interpret. We also findthe 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 fourtimes higher than the average ratio of Arp 220. While there is a possibilitythat the [CI] (1-0) and CO (1-0) emission traces different components, wesuggest that the high line ratios are likely because of elevated CI/COabundance ratios based on our radiative transfer analysis. A CI-rich andCO-poor gas phase in outflows could be caused by the irradiation of the cosmicrays, the shock heating, and the intense radiation field.

Spatially-resolved relation between [CI] $^{3}P_{1}$-$^{3}P_{0}$ and $^{12}$CO (1-0) in Arp 220