Ratio of star intensity to the THEMIS ISRF at the core position, and ratio of the observed core and rim region intensity to the THEMIS AMMI and AMM models, respectively, as a function of wavelength. The dotted lines denote the limits for a factor of two uncertainty. The class I protostar intensity at the core is negligible at optical and NIR wavelengths but dominates at the mid-IR and far-IR wavelengths. The ratio of observed core and rim intensities to THEMIS model intensities for AMMI and AMM dust grains, respectively, shows agreement within a factor of two. The high column density at the B207 core results in FIR core intensities higher than the THEMIS AMMI predicted values by a corresponding factor.