GMC Collisions as Triggers of Star Formation. V. Observational Signatures
Abstract
We present calculations of molecular, atomic, and ionic line emission from simulations of giant molecular cloud (GMC) collisions. We post-process snapshots of the magnetohydrodynamical simulations presented in an earlier paper in this series by Wu et al. of colliding and non-colliding GMCs. Using photodissociation region (PDR) chemistry and radiative transfer, we calculate the level populations and emission properties of the transitions of 12CO J = 1-0, [C I] {}3{{{P}}}1\to {}3{{{P}}}0 at 609 μm, [C II] 158 μm, and [O I] {}3{{{P}}}1\to {}3{{{P}}}0 at 63 μm. From emission maps of integrated intensity and position-velocity diagrams, we find that fine-structure lines, particularly [C II] 158 μm, can be used as a diagnostic tracer for cloud-cloud collision activity. These results hold even in more evolved systems in which the collision signature in molecular lines has been diminished.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- November 2017
- DOI:
- 10.3847/1538-4357/aa94c5
- arXiv:
- arXiv:1706.07006
- Bibcode:
- 2017ApJ...850...23B
- Keywords:
-
- ISM: clouds;
- ISM: kinematics and dynamics;
- ISM: lines and bands;
- ISM: magnetic fields;
- ISM: structure;
- methods: numerical;
- Astrophysics - Astrophysics of Galaxies;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 10 pages, 7 figures, accepted for publication in ApJ, comments welcome