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The interstellar molecular clouds are the site of star formation and also thetarget for the cosmic ray protons to produce \gamma-rays via the hadronicprocess. The interstellar atomic gas is enveloping the molecular clouds and mayalso be dense enough to affect the \gamma-ray production. In this Chapter, someof the basic properties of the interstellar gas both in molecular and atomicforms will be reviewed. Then, it is presented that two young TeV \gamma-raySNRs, RX J1713.7-3946 and RX J0852.0-4622, show good spatial correspondencebetween the \gamma-rays and the interstellar protons. The good spatialcorrespondence provides a support for the hadronic origin of the \gamma-rays inthese SNRs. It is emphasized that both molecular and atomic hydrogen plays arole as targets for cosmic ray (CR) protons. The clumpy distribution of thetarget interstellar medium (ISM) protons is crucial in the interaction of thesupernova shocks with the ISM, whereas models with uniform ISM distribution arenot viable. Finally, it is suggested that the dense atomic gas withoutmolecules may occupy the dominant part of the dark gas in the local ISM.

Molecular and atomic gas in the young TeV \gamma-ray SNRs RX J1713.7-3946 and RX J0852.0-4622; evidence for the hadronic production of \gamma-rays