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Fukui et al. (2021) quantified the hadronic and leptonic gamma rays in theyoung TeV gamma ray shell-type supernova remnant (SNR) RXJ1713.7-3946(RXJ1713), and demonstrated that the gamma rays are a combination of thehadronic and leptonic gamma ray components with a ratio of $\sim 6:4$ in gammaray counts $N_\mathrm{g}$. This discovery, which adopted a new methodology ofmultiple-linear gamma-ray decomposition, was the first quantification of thetwo gamma ray components. In the present work, we applied the same methodologyto another TeV gamma ray shell-type SNR RX~J0852.0$-$4622 (RXJ0852) in the 3Dspace characterized by [the interstellar proton column density$N_{\mathrm{p}}$]-[the nonthermal X-ray count$N_{\mathrm{x}}$]-[$N_{\mathrm{g}}$], and quantified the hadronic and leptonicgamma ray components to have a ratio of $\sim 5:5$ in $N_{\mathrm{g}}$. Thepresent work adopted fitting of two/three flat planes in the 3D space insteadof a single flat plane, which allowed to suppress fitting errors. Thequantification indicates that the hadronic and leptonic gamma rays are in thesame order of magnitude in these two core-collapse SNRs, verifying thesignificant hadronic gamma ray components. We argue that the targetinterstellar protons, in particular their spatial distribution, are essentialin any attempts to identify type of particles responsible for the gamma-rayemission. The present results confirm that the CR energy $\lesssim 100$\,TeV iscompatible with a scheme that SNRs are the dominant source of these GalacticCRs.

The Gamma Ray Origin in RXJ0852.0-4622 Quantifying the Hadronic and  Leptonic Components: Further Evidence for the Cosmic Ray Acceleration in  Young Shell-type SNRs