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Fig. 7
z distribution of the Hi-GAL protostars in the ℓ = 30° and ℓ = 59° fields. The z value adopted to estimate the tile volumes is the FWHM of the Gaussian fit. The second peak at z ~ 60 pc in ℓ = 59° is due to a concentration of YSOs in the Vulpecula OB association (Billot et al. 2010).
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