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Herein, we present results from observations of the 12CO (J=1-0), 13CO(J=1-0), and 12CO (J=2-1) emission lines toward the Carina nebula complex (CNC)obtained with the Mopra and NANTEN2 telescopes. We focused onmassive-star-forming regions associated with the CNC including the three starclusters Tr14, Tr15, and Tr16, and the isolated WR-star HD92740. We found thatthe molecular clouds in the CNC are separated into mainly four clouds atvelocities -27, -20, -14, and -8 km/s. Their masses are 0.7x10^4Msun, 5.0x10^4Msun, 1.6x10^4 Msun, and 0.7x10^4 Msun, respectively. Most are likelyassociated with the star clusters, because of their high 12CO (J=2-1)/12CO(J=1-0) intensity ratios and their correspondence to the Spitzer 8 microndistributions. In addition, these clouds show the observational signatures ofcloud--cloud collisions. In particular, there is a V-shaped structure in theposition--velocity diagram and a complementary spatial distribution between the-20 km/s cloud and the -14 km/s cloud. Based on these observational signatures,we propose a scenario wherein the formation of massive stars in the clusterswas triggered by a collision between the two clouds. By using the path lengthof the collision and the assumed velocity separation, we estimate the timescaleof the collision to be ~1 Myr. This is comparable to the ages of the clustersestimated in previous studies.

Massive star formation in the Carina nebula complex and Gum 31 -- I. The Carina nebula complex