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We made CO ($J$ = 1--0, 2--1, and 3--2) observations toward an H{\sc ii}region RCW~32 in the Vela Molecular Ridge. The CO gas distribution associatedwith the H{\sc ii} region was revealed for the first time at a high resolutionof 22 arcsec. The results revealed three distinct velocity components whichshow correspondence with the optical dark lanes and/or H$\alpha$ distribution.Two of the components show complementary spatial distribution which suggestscollisional interaction between them at a relative velocity of $\sim$4km~s$^{-1}$. Based on these results, we present a hypothesis that cloud-cloudcollision determined the cloud distribution and triggered formation of theexciting star ionizing RCW~32. The collision time scale is estimated from thecloud size and the velocity separation to be $\sim$2 Myrs and the collisionterminated $\sim$1 Myr ago, which is consistent with an age of the excitingstar and the associated cluster. By combing the previous works on the H{\sc ii}regions in the Vela Molecular Ridge, we argue that the majority, at least four,of the H{\sc ii} regions in the Ridge were formed by triggering of cloud-cloudcollision.

Detailed CO ($J$ = 1--0, 2--1 and 3--2) observations toward an H{\sc ii} region RCW~32 in the Vela Molecular Ridge