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We present calculations of molecular, atomic and ionic line emission fromsimulations of giant molecular cloud (GMC) collisions. We post-processsnapshots of the magneto-hydrodynamical simulations presented in an earlierpaper in this series by Wu et al. (2017) of colliding and non-colliding GMCs.Using photodissociation region (PDR) chemistry and radiative transfer wecalculate the level populations and emission properties of $^{12}$CO $J=1-0$,[CI] $^3{\rm  P}_1\rightarrow{^3{\rm P}}_0$ at $609\,\mu$m, [CII] $158\,\mu$m and [OI]$^3{\rm P}_1\rightarrow{^3{\rm P}}_0$ transition at $63\,\mu$m. From integratedintensity emission maps and position-velocity diagrams, we find thatfine-structure lines, particularly the [CII] $158\,\mu$m, can be used as adiagnostic tracer for cloud-cloud collision activity. These results hold evenin more evolved systems in which the collision signature in molecular lines hasbeen diminished.

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