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We review recent progress in elucidating the relationship between high-energyradiation and the interstellar medium (ISM) in young supernova remnants (SNRs)with ages of $\sim$2000 yr, focusing in particular on RX J1713.7$-$3946 and RCW86. Both SNRs emit strong nonthermal X-rays and TeV $\gamma$-rays, and theycontain clumpy distributions of interstellar gas that includes both atomic andmolecular hydrogen. We find that shock-cloud interactions provide a viableexplanation for the spatial correlation between the X-rays and ISM. In theseinteractions, the supernova shocks hit the typically pc-scale dense cores,generating a highly turbulent velocity field that amplifies the magnetic fieldup to 0.1-1 mG. This amplification leads to enhanced nonthermal synchrotronemission around the clumps, whereas the cosmic-ray electrons do not penetratethe clumps. Accordingly, the nonthermal X-rays exhibit a spatial distributionsimilar to that of the ISM on the pc scale, while they are anticorrelated atsub-pc scales. These results predict that hadronic $\gamma$-rays can be emittedfrom the dense cores, resulting in a spatial correspondence between the$\gamma$-rays and the ISM. The current pc-scale resolution of $\gamma$-rayobservations is too low to resolve this correspondence. Future $\gamma$-rayobservations with the Cherenkov Telescope Array will be able to resolve thesub-pc-scale $\gamma$-ray distribution and provide clues to the origin of thesecosmic $\gamma$-rays.

The interstellar medium in young supernova remnants: key to the production of cosmic X-rays and $\gamma$-rays