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Fig. 4

image

Spectral energy distributions starless cores (upper) and protostellar envelopes (lower). Shown are the background-subtracted fluxes for the isolated models (left) and their embedded variants (right). Subscripts of the curve labels (F30 to F0.03) indicate the model mass (in M). For protostellar envelopes of the same mass, the SEDs with higher fluxes correspond to higher accretion luminosities L (0.03, 0.1, 0.3, 1, 3, 10, 30 L). Dashed lines indicate the fluxes of the ISRF that were integrated over the projected area of either the isolated models or the embedding clouds.

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