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We present a detailed morphological study of TeV gamma rays, synchrotronradiation, and interstellar gas in the young Type Ia supernova remnant (SNR)RCW 86. We find that the interstellar atomic gas shows good spatial correlationwith the gamma rays, indicating that the TeV gamma rays from RCW 86 are likelyto be dominantly of hadronic origin. In contrast, the spatial correlationbetween the interstellar molecular cloud and the TeV gamma rays is poor in thesoutheastern shell of the SNR. We argue that this poor correlation can beattributed to the low-energy cosmic rays (~ 1 TeV) not penetrating into thedense molecular cloud due to an enhancement of the turbulent magnetic fieldaround the dense cloud of ~ 10-100 $\mu$G. We also find that the southwesternshell, which is bright in both synchrotron X-ray and radio continuum radiation,shows a significant gamma-ray excess compared with the interstellar protoncolumn density, suggesting that leptonic gamma rays via inverse Comptonscattering possibly contributes along with hadronic gamma rays. The totalcosmic-ray energies of the young TeV gamma-ray SNRs$-$RX J1713.7$-$3946, VelaJr, HESS J1731$-$347, and RCW 86$-$are roughly similar, which indicates thatcosmic rays can be accelerated in both the core-collapse and Type Iasupernovae. The total energy of cosmic rays derived using the gas density, ~10$^{48}$-10$^{49}$ erg, gives a safe lower limit due mainly to the low fillingfactor of interstellar gas within the shell.

Possible Evidence for Cosmic-Ray Acceleration in the Type Ia SNR RCW 86: Spatial Correlation between TeV Gamma rays and Interstellar Atomic Protons