Table 1
Sample of massive dense clumps and general properties.
| Source | RA; Dec (J2000) | l;b | da | θsa | Mgasb | Tkb | N(H_2)b | Σ(H2)b | fCOc | σnthd | Rec. fluxe | SFE |
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| h m s;°′′′ | °;° | kpc | ′′ | M⊙ | K | 1023 cm−2 | g cm−2 | km s−1 | Jy/Jy | % | ||
| 08477−4359c1f | 08:49:35.13;−44:11:59 | 264.69;−0.07 | 1.8 | 35.6 | 86.73 | 19 | 1.42 | 0.24 | 7 | 1.03 | 0.12/0.62 | –g |
| 13039−6108c6 | 13:07:14.80;−61:22:55 | 305.18;1.14 | 2.4 | 40.3 | 101.5 | 17 | 0.68 | 0.12 | 22 | – | 0 | –g |
| 15470−5419c1 | 15:51:28.24;−54:31:42 | 327.51;−0.83 | 4.1 | 24.2 | 310.2 | 18 | 1.37 | 0.36 | 35 | 1.02 | 0.01/0.56 | 6% |
| 15470−5419c3f | 15:51:01.62;−54:26:46 | 327.51;−0.72 | 4.1 | 54.1 | 743.4 | 19 | 1.11 | 0.17 | 36 | 1.13 | 0.09/0.50 | 3% |
| 15557−5215c2f | 15:59:36.20;−52:22:58 | 329.81;0.03 | 4.4 | 41.3 | 633.4 | 23 | 1.55 | 0.22 | 32 | 0.96 | 0.12/0.90 | 4% |
| 15557−5215c3 | 15:59:39.70;−52:25:14 | 329.80;0.00 | 4.4 | 35.8 | 194.3 | 15 | 0.49 | 0.09 | 24 | – | 0 | 8% |
| 16061−5048c1f | 16:10:06.61;−50:50:29 | 332.06;0.08 | 3.6 | 28.1 | 284.3 | 25 | 1.66 | 0.31 | 12 | 1.52 | 0.63/1.02 | 31% |
| 16061−5048c4 | 16:10:06.61;−50:57:09 | 331.98;0.00 | 3.6 | 62.8 | 504.2 | 13 | 1.22 | 0.11 | 34 | 0.82 | 0.03/0.32 | 3% |
| 16435−4515c3 | 16:47:33.13;−45:22:51 | 340.31;−0.71 | 3.1 | 17.7 | 147 | 12 | 1.20 | 0.55 | 73 | – | 0 | 11% |
| 16482−4443c2 | 16:51:44.59;−44:46:50 | 341.24;−0.90 | 3.7 | ≪ 24h | 59.08 | 16 | ≫ 4.63h | 0.66 | 9 | 1.40 | 0.07/0.23 | 17% |
| 16573−4214c2 | 17:00:33.38;−42:25:18 | 344.08;−0.67 | 2.6 | 7.29 | 108.3 | 17 | 1.89 | 3.4 | 25 | 1.17 | 0.07/0.71 | 14% |
Notes. The table lists: coordinates, distance, deconvolved angular diameter, gas mass, gas temperature, H2 column density, mass surface density, CO depletion factor, and non-thermal velocity dispersion (parameters taken or derived from Beltrán et al. 2006; Fontani et al. 2012; Giannetti et al. 2013). In the last two columns, we give the recovered flux in the ALMA images, and the star formation efficiency (SFE), computed as explained in Sect. 2. (a) From Beltrán et al. (2006); (b) from Giannetti et al. (2013); (c)from Fontani et al. (2012); (d)derived from the C18O (3–2) line width at half maximum (Fontani et al. 2012) by subtracting the thermal contribution calculated according to the gas temperature in Col. 7; (e)ratio between thetotal flux integrated inside the ALMA primary beam, and the peak flux of the SIMBA map towards the phase centre. The SIMBA main beam and the ALMA primary beam are the same (~ 24′′), and the fluxratios were compared by correcting the SIMBA flux at 250 GHz assuming a spectral index β = 2; (f) detected in the Spitzer 24 μm image (Fig. 1); (g)it is not possible to derive the SFE because the bolometric luminosity is not available (Giannetti et al. 2013); (h) point-like source in the SIMBA 1.2 mm map (Beltrán et al. 2006).
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