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In the line-of-sight toward the DO-type white dwarf RX J0503.9-2854, thedensity of the interstellar medium (ISM) is very low, and thus thecontamination of the stellar spectrum almost negligible. This allows us toidentify many metal lines in a wide wavelength range from the extremeultraviolet to the near infrared. In previous spectral analyses, many metallines in the ultraviolet spectrum of RX J0503.9-2854 have been identified. Acomplete line list of observed and identified lines is presented here. Wecompared synthetic spectra that had been calculated from model atmospheres innon-local thermodynamical equilibrium, with observations. In total, weidentified 1272 lines (279 of them were newly assigned) in the wavelength rangefrom the extreme ultraviolet to the near infrared. 287 lines remainunidentified. A close inspection of the EUV shows that still no good fit to theobserved shape of the stellar continuum flux can be achieved although He, C, N,O, Al, Si, P, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Cr, Ni Zn, Ga, Ge, As, Kr, Zr, Mo,Sn, Xe, and Ba are included in the stellar atmosphere models. There are twopossible reasons for the deviation between observed and synthetic flux in theEUV. Opacities from hitherto unconsidered elements in the model-atmospherecalculation may be missing and/or the effective temperature is slightly lowerthan previously determined.

Complete spectral energy distribution of the hot, helium-rich white dwarf RX J0503.9-2854