Notes. ⁽¹⁾ Position of the maximum emission of the cores. The coordinates have an error of approximately 1 arcsec (pointing rms, but each APEX/LABOCA cell has a 4 arcsec size). ⁽²⁾ APEX/LABOCA flux density at 870 μm computed above 3σ emission. The absolute uncertainty in the flux scale is 8%. ⁽³⁾ APEX/LABOCA peak intensity at 870 μm (maximum of the emission). For point-like sources, the value is equal to the previous column. ⁽⁴⁾ Values derived from the extinction map, with a resolution of 1.5 arcmin, three times larger the LABOCA beam-size. ⁽⁵⁾ Envelope masses derived using the 870 μm flux densities and assuming a dust temperature of 15 K (Sánchez-Monge et al. 2013), and a dust (and gas) mass opacity coefficient of 0.0175 cm² g⁻¹ (obtained by interpolating the tabulated values of Ossenkopf & Henning 1994, see Sect. 3.1). The uncertainty in the masses due to the dust temperature and opacity law is estimated to be a factor of 4. ⁽⁶⁾ Internal luminosity of the core, based on MIPS flux at 70 μm, after Dunham et al. (2008). ⁽⁷⁾ Deconvolved size after fitting a Gaussian to the cores. The averaged of the major and minor axis is represented. “PL” stands for point-like source. ⁽⁸⁾ Gr = groups 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; B2 = upper limit both at 70 and 24 μm; C1 = no data at 70 μm and detection at 24 μm; C2 = no data at 70 μm and upper limit at 24 μm. ⁽⁹⁾ Tentative classification: YSO = young stellar object, with a optical and/or near-IR 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 near-IR 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 an optical/IR source farther away with excess. ⁽¹⁰⁾ Presence of BD candidates: the first column indicates whether there is a BD candidate within APEX/LABOCA beam, whereas the second column indicates whether there is a optical/IR counterpart within 5 arcsec from APEX/LABOCA peak (the letter for the identification and the “BD” super-index for the substellar candidates). ^(a) B30-LB03 and B30-LB04 very close to each other, see Sect. A.1. ^(b) IRAS 05286+1203, RA = 82.8671, Dec = +12.0899, [12] = 7.79e − 01 ± 0.0779 Jy, [25] = 1.91e + 00 ± 0.2101 Jy, [60] = 9.35e + 00 ± 1.7765 Jy, [100] = 7.04e + 01 ± 14.784 Jy. LB30-LB19d has a MIPS 2 flux at 70 μm of 0.200 Jy, which translate to L(∫) = 0.094 L_⊙ (i.e., a VeLLO). Note that within the LABOCA beam there is a APEX/SABOCA source detected at 350 μm (B30-SB08, Huélamo et al. 2017). ^(c) B30-LB20 contains a APEX/SABOCA at 350 μm (B30-SB09, Huélamo et al. 2017). ^(d) There are two APEX/SABOCA sources within the B30-LB22 beam (B30-SB03 and B30-SB04, Huélamo et al. 2017). ^(e) There are two APEX/SABOCA sources within the B30-LB23 beam (B30-SB05 and B30-SB06, Huélamo et al. 2017). ^(f) B30-LB27 contains a APEX/SABOCA at 350 μm (B30-SB12, Huélamo et al. 2017). ^(g) B30-LB28 contains a APEX/SABOCA at 350 μm (B30-SB16, Huélamo et al. 2017). ^(h) IRAS 05293+1207, RA = 83.0450, Dec = +12.1629, [12] < 2.50e − 01 Jy, [25] < 2.71e − 01 Jy, [60] = 1.15e + 00 ± 0.1725 Jy, [100] < 2.66e + 01 Jy. ⁽ⁱ⁾ B30-LB33 and B30-LB34 very close to each other, see Sect. A.1. ^(j) The MIPS M2 flux probably corresponds to the counterpart identified as LB25c. ^(*) Extended emission at 24 μm.