Raman-scattering by atomic hydrogen is a unique spectroscopic process that may probe the mass transfer and mass loss phenomena in symbiotic stars(SSs). In the optical high resolution spectra of the S-type SS V455 Sco, we note the presence of two Raman-scattered features, one at around 6825 angstrom with a triple-peak profile formed from Raman-scattering of O VI lambda 1032 and the other Raman-scattered He II lambda 1025 at around 6545 angstrom. Adopting an accretion flow model with additional contribution from a collimated bipolar outflow, we propose that the blue and central peaks are contributed from the accretion flow and the bipolar flow is responsible for the remaining red peak. With the absence of [N II] lambda 6548, the Raman-scattered He II lambda 1025 at around 6545 angstrom is immersed in the broad Ha wings that appear to be formed by Raman-scattering of far-UV continuum near Lyman series.