RNe SEDs. These are effectively low-resolution spectra of 10 RNe, with the flux density (in jansky) as a function of the light frequency (in Hertz) on a log–log plot. The error bars are dominated by the uncertainty in the extinction, and are correlated from point to point for a given RN, so that a curve following the upper end of the error bars represents the lowest extinction case and the curve that follows the lower end of the error bars represents the highest extinction case. For V3890 Sgr, V745 Sco, T CrB, and RS Oph, we see a broad peak around log(ν) from 14.3 to 14.4 (corresponding to temperatures of ~3800°) produced by the early M giant companion star. For T Pyx, IM Nor, CI Aql, V2487 Oph, and U Sco, we see the expected f _ν ∝ ν ^1/3 behavior for an accretion disk.