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Fig. 6


Lbol versus Tbol after Young & Evans (2005) and Dunham et al. (2008). Sources compiled in these two works, with evidences for being embedded low luminosity sources, are shown as solid black squares. Young members from Tobin et al. (2016) in Perseus are displayed as open squares. The black crosses correspond to Taurus members in Chen et al. (1995), whereas solid, black circles comefrom Bayo et al. (2011) and the Collinder 69 cluster. The cyan, short-dashed lines show the evolutionary tracks for the three models with different masses (in solar masses) considered by Young & Evans (2005). The magenta, dotted and long-dashed lines show the evolutionary tracks for three models considered by Myers et al. (1998). The blue solid lines correspond to isochrones by Baraffe et al. (1998). The vertical dashed lines show the Class 0–I and Class I–II Tbol boundaries from Chen et al. (1995). The big, labeled circles correspond to several counterparts for our B30 sources detected at 70 μm (our group A). Green with detections at 24 μm and cyan undetected at that band. Solid (green or cyan) circles denote counterparts whose properties have been derived with the 870 μm flux (for counterparts assumed to the primary origin of the submm emission), whereas open symbols represent values estimated without this flux, and the arrows move their location to the values derived when including this value.

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