  We present our spectroscopic data around H$\beta$ of the symbiotic star V1016
Cyg obtained with the Bohyunsan Echelle Spectrograph, in order to secure the
broad emission feature at around 4850\AA, which is formed through Raman
scattering of He II $\lambda$ 972. The total cross section around Ly$\gamma$ is
approximately given by $\sigma(\lambda)\simeq 1.7\times
10^{-28}[\lambda_{Ly\gamma}/(\lambda -\lambda_{Ly\gamma})]^2{\rm cm^2}$, with
$\lambda_{Ly\gamma}$ being the line centre wavelength of Ly$\gamma$. We find a
centre shift redward by an amount $\Delta\lambda= +0.64{\rm \AA}$ in the Raman
scattered He II $\lambda$ 4850. This redward centre shift is exactly analogous
to the effect for the Raman scattered He II $\lambda$ 6545 blueward of
H$\alpha$ discussed in our previous study. We compute the branching ratios of
Raman scattering into the level $2s$ and levels $3s,$ and 3d, which are
subsequently incorporated in our Monte Carlo code. Assuming that He II
$\lambda$ 972 emission is characterized by a single Gaussian profile, the
redward peak shift observed in the Raman scattered He II 4850 feature
corresponds to the neutral column density $N_{HI}=1.2\times 10^{21}{\rm\
cm^{-2}}$. Assuming that the covering factor $\sim 0.1$ of the scattering
region with respect to the He II emission region and adopting a simple
spherical stellar wind model, we may place an upper bound $\dot M \le 3.6\times
10^{-7}{\rm M_\odot yr^{-1}}$ for the mass loss rate of the giant component of
V1016 Cyg. Our estimate can be severely affected by the inematics of the
scattering and He II emission regions and the exact atomic physics, about which
brief discussions are presented.
