Notes. ⁽¹⁾ Grouping based on the detection at 70 and 24 μm and presence of counterparts, as discussed in Sect. 2.7: A1 = Detection at 70 and 24 μm; A2 = detection at 70 and upper limit at 24 μm; B1 = upper limit at 70 μm and detection at 24 μm; C1 = no data at 70 μm and detection at 24 μm. Objects without detected emision at 24 and/or 70 μm are not listed here (B2 and C2). Tentative classification: YSO = Young Stellar Object, with a optical and/or nearIR sources within 5 arcsec of APEX/LABOCA central coordinate. Our tentative interpretation is that most of them are proto-stars or proto-BDs. Excess = Optical and/or nearIR sources with excesses within the APEX/LABOCA beam but farther than 5 arcsec. The submm source cannot be assigned unambiguously to any counterpart so its nature remains unknown. Starless = Possible starless core, since there is neither counterparts closer than 5 arcsec nor a optical/IR source farther away with excess. ⁽²⁾ Including the flux at 870 μm from APEX/LABOCA and, if present, MIPS M2. ⁽³⁾ Internal luminosity, based on MIPS flux at 70 μm, after Dunham et al. (2008). ⁽⁴⁾ SED classification based on the T_bol versus L_bol diagram. ⁽⁵⁾ There is a submm source nearby, namely SB08, detected with APEX/SABOCA at 350 μm (Huélamo et al. 2017). ⁽⁶⁾ There is a submm source nearby, namely SB05, detected with APEX/SABOCA at 350 μm (Huélamo et al. 2017). ⁽⁷⁾ There is a submm source nearby, namely SB04, detected with APEX/SABOCA at 350 μm (Huélamo et al. 2017). ⁽⁸⁾ There is a submm source nearby, namely SB03, detected with APEX/SABOCA at 350 μm (Huélamo et al. 2017). ^(†) Membership status updated from Table 7 to Y? based on all the available data and our analysis. ^(*) Possible detection at MIPS 24 μm, but if real, it might be affected by the inhomogeneous extended emission by the nebulosity.