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

Abstract

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 $2.62\times 10^{-22}\mathrm{c}{\mathrm{m}}^2$ 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 $\sim 20\mathrm{km}{\mathrm{s}}^{-1}$ in 2005.

8 pages, 8 figures, accepted for publication in MNRAS

References in corpus (2)

• Broad H-alpha wings from the optically thin stellar wind of the hot components in symbiotic binaries
• Raman Scattered O VI $\lambda$ 6825 and the Accretion Disk Emission Model in the Symbiotic Stars V1016 Cygni and HM Sagittae

Cited by in corpus (2)

• Discovery of true, likely and possible symbiotic stars in the dwarf spheroidal NGC 205
• RAMSES II - RAMan Search for Extragalactic Symbiotic Stars. Project concept, commissioning, and early results from the science verification phase