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Interstellar molecular clouds are gamma ray sources through the interactionswith cosmic ray protons followed by production of neutral pions which decayinto gamma rays. We present new NANTEN2 observations of the TeV gamma ray SNRRXJ1713.7-3946 and the W28 region in the 12CO J=2-1, 4-3 and 7-6 emissionlines. In RXJ1713.7-3946 we confirm that the local molecular gas havingvelocities around -10 km/s shows remarkably good spatial correlations with theSNR. We show that the X ray peaks are well correlated with the molecular gasover the whole SNR and suggest that the interactions between the SNR and themolecular gas play an important role in cosmic ray acceleration via severalways including magnetic field compression. The CO J=4-3 distribution towardspeak C shows a compact and dense cloud core having a size of about 1 pc as wellas a broad wing. The core shows a notable anti-correlation with the Suzaku Xray image and is also associated with hard gamma rays as observed with HESS.Based on these findings, we present a picture that peak C is a molecular clumpsurvived against the impact of the SN blast waves and is surrounded by highenergy electrons emitting the X ray. The TeV gamma ray distribution is, on theother hand, more extended into the molecular gas, supporting the hadronicorigin of gamma ray production. W28 is one of the most outstanding star formingregions exhibiting TeV gamma rays as identified through a comparison betweenthe NANTEN CO dataset and HESS gamma ray sources. In the W28 region, we showthe CO J=2-1 distribution over the whole region as well as the detailed imageof the two TeV gamma ray peaks. One of them show strong CO J=7-6 emission,suggesting high excitation conditions in this high mass star forming core. Apursuit for the detailed mechanism to produce gamma rays is in progress.

Sub-mm/mm studies of the molecular gas in the Galactic disk; the TeV gamma ray SNR RXJ1713.7-3946 and the W28 high mass star forming region