  The young planetary nebula NGC 6302 is known to exhibit Raman-scattered He II
features at 6545 and 4851 Angstrom. These features are formed through inelastic
scattering of He II$\lambda\lambda$ 1025 and 972 with hydrogen atoms in the
ground state, for which the cross sections are $1.2 \times 10^{-21}$ and
$1.4\times 10^{-22} {\rm\ cm^2}$, respectively. We investigate the spectrum of
NGC 6302 archived in the ESO Science Portal. Our Gaussian line fitting analysis
shows that the Raman-scattered He II features are broader and more redshifted
than the hypothetical model Raman features that would be formed in a cold
static H I medium. We adopt a simple scattering geometry consisting of a
compact He II emission region surrounded by a H I medium to perform Monte Carlo
simulations using the radiative transfer code ${\it STaRS}$. Our simulations
show that the H I region is characterized by the H I column density $N_{\rm
HI}=3\times 10^{21}{\rm\ cm^{-2}}$ with the random speed component $v_{\rm
ran}=10{\rm\ km\ s^{-1}}$ expanding with a speed $v_{\rm exp}= 13{\rm\ km\
s^{-1}}$ from the He II emission region. Based on our best fit parameters, we
estimate the H I mass of the neutral medium $M_{\rm HI} \simeq 1.0\times
10^{-2}\ {\rm M_\odot}$, pointing out the usefulness of Raman He II
spectroscopy as a tool to trace H I components.
