Fig. 12
The SEDs of massive-star forming regions associated with massive clumps detected in 1.2 mm continuum emission; top labels show names of the clumps. Dots with error bars are flux densities estimated from SIMBA, IRAS, and MSX observations. Each SED is modeled with two dust components at different temperatures (physical parameters for each model are in Table 4); drawn lines are the total flux density of the two dust components, and dashed lines are the contributions of each dust component.
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