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We present the high resolution spectra of the symbiotic star V1016 Cygniobtained with the Bohyunsan Optical Echelle Spectrograph in 2003 and 2005, fromwhich we find a broad emission feature at 4881 \AA. We propose that this broadfeature is formed from Raman scattering of Ne VII$\lambda973$ by atomichydrogen. Thus far, the detection of Raman scattered lines by atomic hydrogenis limited to O VI$\lambda\lambda$1032, 1038 and He II$\lambda\lambda$940, 972and 1025. With the adoption of the center wavelength 973.302 \AA\ of NeVII$\lambda$973 and consideration of the air refractive index of$n_{air}=1.000279348$, the atomic line center of the Raman scattered Ne VIIfeature is determined to be 4880.53 \AA. The total cross section at the linecenter of Ne VII$\lambda973$ is computed to be $2.62\times 10^{-22}{\rm\ cm^2}$with the branching ratio of 0.17. We perform Monte Carlo simulations to fit theRaman scattered Ne VII$\lambda973$. Assuming that the Ne VII and He II emissionregions share the same kinematics with respect to the neutral scatteringregion, we find that the Raman scattered He II$\lambda$972 at 4850 \AA\ and NeVII$\lambda$973 at 4881 \AA\ are excellently fitted. We also propose that theHe II and Ne VII emission regions were stationary with respect to the H Iregion in 2003 but that they were receding from it with a velocity $\sim20{\rm\ km\ s^{-1}}$ in 2005.

Raman Scattered Ne VII$\lambda$973 at 4881 \AA\ in the Symbiotic Star V1016 Cygni