Spectral energy distribution (SED) of IRAS 07251−0248 E from λ_rest = 2.6 to 1200 μm and model. In black, the full JWST NIRSpec & MIRI/MRS spectrum is shown, together with Spitzer, Herschel/PACS (from 60 to 160 μm, both photometric and spectroscopic) and SPIRE (from 230 to 470 μm), and ALMA (667 and 1200 μm) data. The colored circles at 667 μm indicate the contributions by the unresolved (blue) and resolved (light-blue) components inferred from the model in Fig. 1. At 1.2 mm, the open black circle and the cross indicate the flux densities of the unresolved (< 82 pc) and resolved (540 × 330 pc²) components, respectively (Pereira-Santaella et al. 2021). The model includes the H_C in blue (dashed: unattenuated emission; solid: attenuated), the W_C in light-blue (extincted), a cold component (C_C) in orange, the stellar component in gray, and the “hidden” component (whose attenuated emission is added to that of the W_C, see Section 3.2) in dotted-dashed green. Red is total. The insert panels show details of the model results. Upper left: The T_dust profile of the H_C. Upper right: The optical depths τ of the H_C and the W_C as function of wavelength. Lower middle: The T_dust profile of the H_C as function of the optical depth from surface at 7 and 14 μm.