Sub-mm [C I] and CO observations of molecular clouds presumably interacting with the G359. 54+0. 18 nonthermal filaments
Abstract
We present new investigations of the physical properties of two molecular clouds, presumably interacting with the G359.54+0.18 Nonthermal Filaments and a possibly associated H region east of the filaments (Staguhn et al., 1997). The data presented here include observations of the sub-mm 490 GHz [CI] 3P1->3P0 transition obtained with the sub-mm telescope AST/RO and KOSMA mm and sub-mm observations of 12 CO and 13 CO. We find indications for enhanced temperatures in the dense regions of both clouds. Only the [CI] emission of the molecular cloud which is kinematically linked to the recombination line velocity, observed east of the filaments, shows a pronounced anti correlation with the molecular emission over a large angular extend. It is questionable whether this different appearance of molecular line emission and the emission of atomic carbon can be explained exclusively by a higher abundance of neutral carbon in the surface regions of dense molecular clumps, as can be observed e.g. in typical PDR regions in the Galactic disk.
- Publication:
-
The Central Regions of the Galaxy and Galaxies
- Pub Date:
- 1998
- Bibcode:
- 1998IAUS..184..175S