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Large-scale CO surveys have revealed that the central molecular zone (CMZ) ofour Galaxy is characterized by a number of expanding shells/arcs, and by apeculiar population of compact clouds with large velocity widths --high-velocity compact clouds (HVCCs). We have performed a large-scale CO J=3-2survey of the CMZ from 2005 to 2008 with the Atacama Submillimeter-waveTelescope Experiment (ASTE). The data cover almost the full extent of the CMZand the Clump 2 with a 34 arcsec grid spacing. The CO J=3-2 data were comparedwith the CO J=1--0 data taken with the Nobeyama Radio Observatory 45 mtelescope. Molecular gas in the CMZ exhibits higher J=3-2/J=1-0 intensityratios [R(3-2/1-0)=0.7] than that in the Galactic disk [R(3-2/1-0)=0.4]. Weextracted highly excited, optically thin gas by the criterion, R(3-2/1-0)>=1.5.Clumps of high R(3-2/1-0) gas were found in the Sgr A and Sgr C regions, nearSNR G 0.9+0.1, and three regions with energetic HVCCs; CO 1.27+0.01, CO-0.41-0.23, and CO -1.21-0.12. We also found a number of small spots of highR(3-2/1-0) gas over the CMZ. Many of these high R(3-2/1-0) clumps and spotshave large velocity widths, and some apparently coincides with HVCCs,suggesting that they are spots of shocked molecular gas. Their origin should belocal explosive events, possibly supernova explosions. These suggest that theenergetic HVCCs are associated with massive compact clusters, which have beenformed by microbursts of star formation. Rough estimates of the energy flowfrom large to small scale suggest that the supernova shocks can make asignificant contribution to turbulence activation and gas heating in the CMZ.

The ASTE Galactic Center CO J=3-2 Survey: Probing Shocked Molecular Gas in the CMZ