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We have analyzed the atomic and molecular gas using the 21 cm HI and 2.6/1.3mm CO emissions toward the young supernova remnant (SNR) RCW 86 in order toidentify the interstellar medium with which the shock waves of the SNRinteract. We have found an HI intensity depression in the velocity rangebetween $-46$ and $-28$ km s$^{-1}$ toward the SNR, suggesting a cavity in theinterstellar medium. The HI cavity coincides with the thermal and non-thermalemitting X-ray shell. The thermal X-rays are coincident with the edge of the HIdistribution, which indicates a strong density gradient, while the non-thermalX-rays are found toward the less dense, inner part of the HI cavity. The mostsignificant non-thermal X-rays are seen toward the southwestern part of theshell where the HI gas traces the dense and cold component. We also identifiedCO clouds which are likely interacting with the SNR shock waves in the samevelocity range as the HI, although the CO clouds are distributed only in alimited part of the SNR shell. The most massive cloud is located in thesoutheastern part of the shell, showing detailed correspondence with thethermal X-rays. These CO clouds show an enhanced CO $J$ = 2-1/1-0 intensityratio, suggesting heating/compression by the shock front. We interpret that theshock-cloud interaction enhances non-thermal X-rays in the southwest and thethermal X-rays are emitted by the shock-heated gas of density 10-100 cm$^{-3}$.Moreover, we can clearly see an HI envelope around the CO cloud, suggestingthat the progenitor had a weaker wind than the massive progenitor of thecore-collapse SNR RX J1713.7$-$3949. It seems likely that the progenitor of RCW86 was a system consisting of a white dwarf and a low-mass star withlow-velocity accretion winds.

Interstellar Gas and X-rays toward the Young Supernova Remnant RCW 86; Pursuit of the Origin of the Thermal and Non-Thermal X-ray