Spectral energy distribution for WR 102c. The reddened spectrum of the PoWR model with T_∗ = 75 kK is shown as a red solid line (see Table 3 for the detailed parameters) and compared to the available photometry, which is indicated by blue (UKIDSS) and black (HST NICMOS Paα filters and Spitzer IRAC Channels 2 and 3) boxes. The inset in the upper right corner shows the continuum photometry marks compared to the continuum SED for the two alternative models used in Fig. 6 with T_∗ = 66 kK (green dashed curve) and 75 kK (red solid curve), respectively. The overall SED fit is hardly affected by the temperature uncertainty. We note that in the mid-IR the stellar SED is below the photometric observation, attributed to the emission from a warm dusty nebula (Barniske et al. 2008).