GMC Collisions as Triggers of Star Formation. V. Observational Signatures
Artikel i vetenskaplig tidskrift, 2017

© 2017. The American Astronomical Society. All rights reserved.. 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 12 CO J = 1-0, [C i] at 609 μm, [C ii] 158 μm, and [O i] 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.

magnetic fields - ISM

clouds - ISM


structure - methods


lines and bands - ISM

kinematics and dynamics - ISM


T.G. Bisbas

University of Florida

Max-Planck-Institut für extraterrestrische Physik

K.E.I. Tanaka

University of Florida

Jonathan Tan

National Astronomical Observatory of Japan

University of Florida

B. Wu

National Astronomical Observatory of Japan

F. Nakamura

National Astronomical Observatory of Japan

Astrophysical Journal

0004-637X (ISSN) 1538-4357 (eISSN)

Vol. 850 1 23-32


Astronomi, astrofysik och kosmologi


Grundläggande vetenskaper


Onsala rymdobservatorium



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