The Spatial Distribution of Atomic Carbon Emission in the Giant Molecular Cloud NGC 604‐2
Abstract
We have mapped a giant molecular cloud in the giant HII region NGC 604 in M33 in the 492 GHz ^3P_1 -- ^3P_0 transition of neutral atomic carbon using the James Clerk Maxwell Telescope. We find the distribution of the [CI] emission to be asymmetric with respect to the CO J=1--0 emission, with the peak of the [CI] emission offset towards the direction of the center of the HII region. In addition, the line ratio I_{[CI]}/I_{CO} is highest (~ 0.2) facing the HII region and lowest (< 0.1) away from it. These asymmetries indicate an edge-on morphology where the [CI] emission is strongest on the side of the cloud facing the center of the HII region, and not detected at all on the opposite side This suggests that the sources of the incident flux creating C from the dissociation of CO are the massive stars of the HII region. The lowest line ratios are similar to what is observed in Galactic molecular clouds, while the highest are similar to starburst galaxies and other regions of intense star formation. The column density ratio, N(C)/N(H_2) is a few times 10^{-6}, in general agreement with models of photodissociation regions.
Related Papers
- → Atomic carbon emission from photodissociation of CO2(1978)36 cited
- → Molecular Clouds and Star Formation in the Southern H II Regions(1999)72 cited
- Atomic carbon near the molecular cloud/HII region interface in S 140.(1992)
- → The Plaskett Lecture: Star Formation in the Perseus Molecular Cloud(2011)