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GMC Collisions as Triggers of Star Formation. V. Observational Signatures

T.G. Bisbas ; K.E.I. Tanaka ; Jonathan Tan (Institutionen för rymd-, geo- och miljövetenskap, Astronomi och plasmafysik) ; B. Wu ; F. Nakamura
Astrophysical Journal (0004-637X). Vol. 850 (2017), 1, p. 23-32.
[Artikel, refereegranskad vetenskaplig]

© 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.

Nyckelord: clouds - ISM , ISM , kinematics and dynamics - ISM , lines and bands - ISM , magnetic fields - ISM , numerical , structure - methods

Denna post skapades 2017-12-29. Senast ändrad 2018-01-14.
CPL Pubid: 254199


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