A detailed study of the interstellar protons toward the TeV $\gamma$-ray
  SNR RX J0852.0$-$4622 (G266.2$-$1.2, Vela Jr.); a third case of the
  $\gamma$-rays and ISM spatial correspondence
  We present a new analysis of the interstellar protons toward the TeV
$\gamma$-ray SNR RX J0852.0$-$4622 (G266.2$-$1.2, Vela Jr.). We used the
NANTEN2 $^{12}$CO($J$ = 1-0) and ATCA & Parkes HI datasets in order to derive
the molecular and atomic gas associated with the TeV $\gamma$-ray shell of the
SNR. We find that atomic gas over a velocity range from $V_\mathrm{LSR}$ = $-4$
km s$^{-1}$ to 50 km s$^{-1}$ or 60 km s$^{-1}$ is associated with the entire
SNR, while molecular gas is associated with a limited portion of the SNR. The
large velocity dispersion of the HI is ascribed to the expanding motion of a
few HI shells overlapping toward the SNR but is not due to the Galactic
rotation. The total masses of the associated HI and molecular gases are
estimated to be $\sim2.5 \times 10^4 $ $M_{\odot}$ and $\sim10^3$ $M_{\odot}$,
respectively. A comparison with the H.E.S.S. TeV $\gamma$-rays indicates that
the interstellar protons have an average density around 100 cm$^{-3}$ and shows
a good spatial correspondence with the TeV $\gamma$-rays. The total cosmic ray
proton energy is estimated to be $\sim10^{48}$ erg for the hadronic
$\gamma$-ray production, which may still be an underestimate by a factor of a
few due to a small filling factor of the SNR volume by the interstellar
protons. This result presents a third case, after RX J1713.7$-$3946 and HESS
J1731$-$347, of the good spatial correspondence between the TeV $\gamma$-rays
and the interstellar protons, lending further support for a hadronic component
in the $\gamma$-rays from young TeV $\gamma$-ray SNRs.
