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Table 2

APEX/LABOCA sources in Barnard 30.

B30- RA1 Dec1 Mass5 L(int)6 Flux Ang. rms Gr8 Type9 BD?10



ID (870 μm) All Peak 70 μm size7 870 In In
(2000.0) (2000.0) (mJy) (mJy/beam) (mag) (M) (M) (L) (Jy) () (mJy) beam 5
LB01 05 31 13.64 12 22 22.7 182 114 4.109 0.266 0.166 <0.382 <0.89 22 16 B2 Starless
LB02 05 31 32.30 12 19 14.7 68 68 4.141 0.099 0.099 <0.230 <0.52 PL 11 B2 Excess Y
LB03a 05 31 29.20 12 17 22.7 39 39 2.471 0.057 0.057 PL 9 C2 YSO Y aBD
LB04a 05 31 30.56 12 17 18.7 40 40 2.841 0.059 0.059 PL 9 C2 Excess Y
LB05 05 31 29.47 12 14 30.7 56 35 3.064 0.081 0.051 36 77 C2 YSO Y a
LB06 05 31 30.83 12 12 46.7 144 527 4.670 0.210 0.077 49 8 C2 Starless Y
LB07 05 31 32.19 12 11 46.7 36 36 4.415 0.052 0.052 PL 7 C2 YSO Y aBD
LB08 05 31 23.19 12 11 26.7 73 46 2.486 0.106 0.066 1.223 3.07 27 7 A2 YSO a
LB09 05 31 18.55 12 11 26.7 30 30 3.134 0.043 0.043 <0.422 <0.99 PL 7 B2 YSO Y aBD
LB10 05 31 09.55 12 11 02.7 32 33 1.146 0.046 0.046 PL 7 C2 YSO Y aBD
LB11 05 31 10.37 12 10 38.7 32 33 1.844 0.046 0.046 PL 7 C1 Excess Y
LB12 05 31 27.01 12 10 14.7 59 59 2.474 0.087 0.087 PL 7 C1 Excess Y
LB13 05 31 18.55 12 09 58.7 74 59 3.873 0.108 0.086 <0.382 <0.89 23 7 B2 Starless Y
LB14 05 31 19.37 12 09 10.7 35 35 1.984 0.051 0.051 0.276 0.63 PL 7 A1 YSO Y a
LB15 05 31 27.28 12 07 26.7 38 38 2.736 0.056 0.056 <0.406 <0.95 PL 7 B2 Starless
LB16 05 31 30.01 12 07 06.7 36 36 3.115 0.053 0.053 PL 7 C2 Starless Y
LB17 05 31 09.82 12 06 42.7 40 40 3.236 0.059 0.059 PL 7 C2 YSO Y aBD
LB18 05 31 34.92 12 06 22.7 41 41 2.917 0.059 0.059 PL 8 C1 Excess Y
LB19b 05 31 28.10 12 05 30.7 125 793 2.759 0.182 0.116 0.402 0.94 24 7 A1 YSO Y a, b
LB20c 05 31 22.91 12 05 30.7 33 33 1.775 0.048 0.048 <0.592 <1.42 PL 7 B2* Excess Y
LB21 05 31 36.00 12 05 02.7 74 42 3.897 0.108 0.061 62 7 C2* YSO Y aBD
LB22d 05 31 31.64 12 04 14.7 60 60 2.710 0.088 0.088 PL 7 C1 YSO Y aBD
LB23e 05 31 29.19 12 04 38.7 32 32 3.100 0.046 0.046 0.189 0.42 PL 7 A2 Excess Y
LB24 05 31 23.46 12 04 30.7 30 30 2.376 0.044 0.044 <0.604 <1.45 PL 7 B1 Excess Y
LB25 05 31 20.46 12 05 06.7 87 52 1.898 0.126 0.076 0.557j 1.33j 34 8 A2 YSO Y aBD, e
LB26 05 31 17.73 12 05 06.7 40 40 2.960 0.058 0.058 PL 7 C2 Excess Y
LB27f 05 31 13.37 12 05 30.7 191 103 4.232 0.279 0.150 29 7 C2* Excess Y
LB28g 05 31 07.64 12 05 06.7 48 48 3.477 0.071 0.071 <0.573 <1.37 PL 7 B2* Excess Y
LB29 05 31 08.73 12 03 46.7 44 44 3.430 0.064 0.064 0.337 0.78 PL 7 A2* YSO Y aBD
LB30 05 31 13.37 12 03 34.7 84 69 2.840 0.123 0.101 29 7 C1 Excess Y
LB31 05 31 15.28 12 03 38.7 56 56 2.378 0.082 0.082 PL 7 C1 Excess Y
LB32h 05 32 12.56 12 09 54.7 85 85 0.123 0.123 PL 16 C1 YSO a
LB33i 05 30 13.36 12 08 46.7 60 60 0.714 0.087 0.087 PL 16 C1 YSO a
LB34i 05 30 13.36 12 08 58.7 44 44 0.123 0.064 0.064 PL 16 C2 Starless

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.

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