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Fig. 21


The Aquila sub-field (18′  ×  18′) is shown as the observed images ℐλO at 70, 160, 250, 350, 500 μm (left to right, top to bottom) with the extraction ellipses (FWHM) of only measurable sources (F   P > σ   P and F   T > σ   T) overlaid, as well as the composite 3-color RGB image (500, 250, 160 μm) created using the images ℐλM of the deblending shapes of each extracted source (lower-right). The default condition, that a tentative source must be detected in at least two bands, was used. Only the protostars are visible at 70 μm, whereas at 160 μm one starless core appears, the other cold sources becoming clearly visible in the SPIRE bands. For better visibility, the values displayed in the panels are somewhat limited in range; the color coding in the lower-right panel is linear, in all other panels it is a function of the square root of intensity in MJy/sr.

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