In Lee, Kang & Byun (2001) the discovery of Raman scattered 6545 A feature was reported in symbiotic stars and the planetary nebula M2-9. The broad emission feature around 6545 A is formed as a result of Raman scattering of He II n = 6 $ o$ n = 2 photons by atomic hydrogen. In this paper, we introduce a method to compute the equivalent width of He II $lambda$ 1025 line and present an optical spectrum of the symbiotic star RR Telescopii as an example for a detailed illustration. In this spectrum, we pay attention to the broad H$alpha$ wings and the Raman scattered He II 6545 feature. The broad Ha wings are also proposed to be formed through Raman scattering of continuum around Ly$eta$ by Lee (2000), and therefore we propose that the equivalent width of the He II $lambda$ 1025 emission line is obtained by a simple comparison of the strengths of the 6545 feature and the broad H$alpha$ wings. We prepare a template H$alpha$ wing profile from continuum radiation around Ly$eta$ with the neutral scattering region that is supposed to be responsible for the formation of Raman scattered He II 6545 feature. Isolation of the 6545 feature that is blended with [N II] $lambda$ 6548 is made by using the fact that [N II] $lambda$ 6584 is always 3 times stronger than [N II] $lambda$ 6548. We also fit the 6545 feature by a Gaussian which has a width 6.4 times that of the He II $lambda$ 6527 line. A direct comparison of these two features for RR Tel yields the equivalent width $EW_{Hel025} = 2.3{AA}$ of He II $lambda$ 1025 line. Even though this far UV emission line is not directly observable due to heavy interstellar extinction, nearby He II lines such as He II $lambda$ 1085 line may be observed using far UV space instruments, which will verify this calculation and hence the origins of various features occurring in spectra around H$alpha$.