We present the high resolution spectra of the symbiotic star V1016 Cygni obtained with the Bohyunsan Optical Echelle Spectrograph in 2003 and 2005 , from which we find a broad emission feature at 4881 Å .
We propose that this broad feature is formed from Raman scattering of Ne VII \lambda 973 by atomic hydrogen .
Thus far , the detection of Raman scattered lines by atomic hydrogen is limited to O VI \lambda \lambda 1032 , 1038 and He II \lambda \lambda 940 , 972 and 1025 .
With the adoption of the center wavelength 973.302 Å of Ne VII \lambda 973 and consideration of the air refractive index of n _ { air } = 1.000279348 , the atomic line center of the Raman scattered Ne VII feature is determined to be 4880.53 Å .
The total cross section at the line center of Ne VII \lambda 973 is computed to be 2.62 \times 10 ^ { -22 } { cm ^ { 2 } } with the branching ratio of 0.17 .
We perform Monte Carlo simulations to fit the Raman scattered Ne VII \lambda 973 .
Assuming that the Ne VII and He II emission regions share the same kinematics with respect to the neutral scattering region , we find that the Raman scattered He II \lambda 972 at 4850 Å and Ne VII \lambda 973 at 4881 Å are excellently fitted .
We also propose that the He II and Ne VII emission regions were stationary with respect to the H I region in 2003 but that they were receding from it with a velocity \sim 20 { km s ^ { -1 } } in 2005 .