Fluxes of the isolated starless cores (upper) and protostellar envelopes (lower) fitted with the thinbody (left) and modbody (right) models. The fluxes for the 0.03, 0.3, and 3 M⊙ cores and envelopes (with L⋆ = 1 L⊙) from Fig. 4 are shown as black triangles, squares, and circles, respectively. Successful fits (Sect. 3.4) using different subsets Φn of fluxes are indicated by the solid and dashed lines of different widths and colors. The thin black curves show the flux distributions for the isothermal models where the actual model temperatures (Fig. 3) were replaced with their mass-averaged values: Td(r) = TM (16.3,13.2,9.2 K for starless cores and 18.1,15.6,12.3 K for protostellar envelopes).
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