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Coronal Mass Ejections (CMEs) often show different features in differentband-passes. By combining data in white-light (WL) and ultraviolet (UV) bands,we have applied different techniques to derive plasma temperatures, electrondensity, internal radial speed, etc, within a fast CME. They serve as extensivetests of the diagnostic capabilities, developed for the observations providedby future multi-channel coronagraphs (such as Solar Orbiter/Metis, ASO-S/LST,PROBA-3/ASPIICS). The involved data include WL images acquired by SOHO/LASCOcoronagraphs, and intensities measured by SOHO/UVCS at 2.45 R$_{\odot}$ in theUV (H I Ly$\alpha$ and O VI 1032 {AA} lines) and WL channels. Data from theUVCS WL channel have been employed for the first time to measure the CMEposition angle with polarization-ratio technique. Plasma electron and effectivetemperatures of the CME core and void are estimated by combining UV and WLdata. Due to the CME expansion and the possible existence of prominencesegments, the transit of the CME core results in decreases of the electrontemperature down to $10^{5}$ K. The front is observed as a significant dimmingin the Ly$\alpha$ intensity, associated with a line broadening due to plasmaheating and flows along the line-of-sight. The 2D distribution of plasma speedswithin the CME body is reconstructed from LASCO images and employed toconstrain the Doppler dimming of Ly$\alpha$ line, and simulate future CMEobservations by Metis and LST.

Extensive Study of a Coronal Mass Ejection with UV and WL coronagraphs: the need for multi-wavelength observations