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Fig. 5

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Left: high velocity CO J = 3−2 blue- and red-shifted emission (integrated over vlsr ranges of [−30, 0] km s-1 and [18, 48] km s-1, rest vlsr = 8.8 km s-1, and indicated as light blue and red solid contours, respectively) around SMM1 superimposed on an IRAC band-2 image. Outflow components are indicated using the nomenclature of Dionatos et al. (2010b) along with the positions of protostellar sources associated with the outflows. The dashed box delineates the limits of the LH Spitzer maps. Center: CO J = 3−2 emission as in the left panel, along with the H2 S(1) (black) and [FeII] 18 μm (green) line maps. Notice the dimensions of the image in comparison to the details presented in Figs. 1 and 2. H2 emission follows well the pattern of CO lobes Br2 and Bb2 in a N-S orientation, whereas the [FeII] emission, despite its shorter extent, has the same orientation as the Bb1-Br1 CO lobes pointing to the SE-NW direction. Right: Sketch of the proposed outflow structure from SMM1-a and b. The outflow driven by the embedded source (SMM1-a) has an S-shaped pattern extending roughly in the N-S axis indicated with a dashed line and solid colors. The same outflow is most likely associated with the bow-shocks visible in the Spitzer image of the left panel, delineated here as dark red V-shaped structures. The butterfly-like outflow extending in the SE-NW direction (delineated with a dash-dotted line and hatched colors) most likely corresponds to the less embedded, foreground protostar (SMM1-b). The yellow arrows at the base of the outflows show the direction of the atomic jet.

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