Table 1
Parameters of the continuum sources of the 1 mm ALMA observations of G9.62+0.19.
| Core | RA (a) | Dec (a) | IPeak (b) | Integrated flux (c) | a (d) | b (d) | PA (d) | α (e) | β (f) |  (f) |
Mass (f) | λ (g) | |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Offset (′′) | Offset (′′) | (mJy beam−1) | (mJy) | (milliarcsec) | (milliarcsec) | ° | cm−2 | M⊙ | |||||
| MM1a | −4.58 ± 0.04 | 7.56 ± 0.02 | 24.5 ± 2.7 | 114.0 ± 13.0 | 726 ± 4 | 426 ± 7 | 110.6 ± 9.6 | 3.4 ± 0.5 | 1.6 | 2.9 × 1024 | 10 | – | |
| MM1b | −3.93 ± 0.05 | 6.75 ± 0.02 | 21.4 ± 2.7 | 98.0 ± 12.0 | 712 ± 2 | 432 ± 3 | 90 ± 12 | – | – | – | – | – | |
| MM2 | −4.06 ± 0.00 | 4.46 ± 0.00 | 11.0 ± 0.0 | 19.2 ± 0.0 | 374 ± 13 | 138 ± 42 | 117 ± 16 | – | – | – | – | – | |
| MM3a | −0.20 ± 0.00 | 5.06 ± 0.00 | 27.6 ± 2.0 | 221.0 ± 18.0 | 1251 ± 105 | 419 ± 47 | 0.06 ± 0.02 | 3.3 ± 0.3 | 1.5 | 3.5 × 1024 | 21 | 8 | |
| MM3b | −0.25 ± 0.00 | 4.02 ± 0.00 | 23.0 ± 2.7 | 54.4 ± 8.8 | 384 ± 69 | 281 ± 93 | 1.16 ± 0.68 | – | – | – | – | – | |
| MM4a | E | −1.53 ± 0.00 | 3.35 ± 0.00 | 321.6 ± 6.8 | 699.0 ± 20.0 | 402 ± 18 | 238 ± 15 | 58.4 ± 4.5 | 3.8 ± 0.2 | 1.8 | 9.5 × 1024 | 43 | 6 |
| MM4b | E | −1.84 ± 0.03 | 3.25 ± 0.02 | 82.6 ± 5.3 | 508.0 ± 37.0 | 1162 ± 94 | 345 ± 34 | 119.4 ± 2.1 | – | – | – | – | – |
| MM5 | −1.19 ± 0.02 | 2.20 ± 0.01 | 43.1 ± 6.2 | 42.4 ± 6.1 | – | – | – | – | – | – | – | – | |
| MM6a | −0.04 ± 0.00 | 0.13 ± 0.00 | 65.6 ± 1.9 | 64.6 ± 1.8 | – | – | – | – | – | – | – | – | |
| MM6b | 0.40 ± 0.02 | −0.37 ± 0.02 | 14.8 ± 1.9 | 14.6 ± 1.8 | – | – | – | – | – | – | – | – | |
| MM6c | 0.06 ± 0.01 | −0.01 ± 0.02 | 42.6 ± 1.6 | 251.0 ± 11.0 | 1057 ± 50 | 324 ± 24 | 167.3 ± 1.5 | 3.9 ± 0.3 | 2.1 | 5.8 × 1024 | 22 | – | |
| MM7 | G | 0.30 ± 0.01 | −2.30 ± 0.01 | 168.9 ± 11.0 | 321.0 ± 30.0 | 359 ± 45 | 152 ± 82 | 175 ± 15 | 3.8 ± 0.5 | 1.8 | 3.5 × 1025 | 15 | – |
| MM8a | F | 1.32 ± 0.00 | −4.52 ± 0.00 | 366.7 ± 7.5 | 675.0 ± 20.0 | 342 ± 17 | 210 ± 11 | 85.2 ± 4.1 | 3.8 ± 0.3 | 1.8 | 4.7 × 1025 | 38 | 21 |
| MM8b | F | 1.15 ± 0.02 | −4.73 ± 0.04 | 80.7 ± 4.8 | 1011.0 ± 65.0 | 1612 ± 107 | 568 ± 44 | 7.2 ± 2.2 | – | – | – | – | – |
| MM8c | F | 1.25 ± 0.03 | −3.75 ± 0.01 | 44.6 ± 6.9 | 43.9 ± 6.8 | – | – | – | – | – | – | – | – |
| MM9 | 3.51 ± 0.03 | −6.43 ± 0.02 | 63.4 ± 7.6 | 147.0 ± 17.0 | 364 ± 0 | 310 ± 0 | 87.8 ± 0.1 | 3.1 ± 0.7 | 1.3 | 1.9 × 1025 | 23 | – | |
| MM10 | 2.18 ± 0.04 | −6.61 ± 0.03 | 23.0 ± 4.1 | 53.4 ± 9.6 | 402 ± 34 | 259 ± 47 | 36 ± 36 | – | – | – | – | – | |
| MM11a | D | 2.03 ± 0.01 | −8.26 ± 0.03 | 42.8 ± 2.1 | 277.0 ± 15.0 | 1046 ± 62 | 363 ± 32 | 172.1 ± 2.1 | 2.7 ± 0.4 | 0.9 | 8.7 × 1024 | 37 | – |
| MM11b | D | 2.30 ± 0.02 | −8.19 ± 0.01 | 20.3 ± 2.4 | 20.0 ± 2.4 | – | – | – | – | – | – | – | – |
| MM11c | D | 1.91 ± 0.01 | −8.78 ± 0.02 | 17.3 ± 2.4 | 17.1 ± 2.4 | – | – | – | – | – | – | – | – |
| MM12a | 3.20 ± 0.03 | −10.81 ± 0.03 | 6.8 ± 1.4 | 8.7 ± 1.8 | – | – | – | – | – | – | – | – | |
| MM12b | 3.42 ± 0.03 | −11.38 ± 0.04 | 6.2 ± 1.4 | 8.3 ± 1.9 | – | – | – | – | – | – | – | – | |
| MM12c | 3.68 ± 0.03 | −12.16 ± 0.03 | 7.3 ± 1.4 | 10.3 ± 2.0 | – | – | – | – | – | – | – | – | |
Notes. (a) The offsets are relative to the absolute position α2000 = 18h06m14.78s δ2000 =−20°31′34.9′′. (b) Peak flux density. (c)Total flux density from the 2D Gaussian fit. To model MM6, MM8, and MM11 we make use of Gaussian components and point-like source components. CASA task IMFIT was used to perform the Gaussian fit. (d) a, b, and PA are the deconvolved FWHM major and minor axes and position angle, obtained from 2D Gaussian fits. Point sources are those for which a, b, and PA are missing. Uncertainties of 0.00 and 0.0 are <0.01 and < 0.1, respectively. (e) Spectral index α obtained between our ALMA band 7 observations and ALMA band 6 observations by Liu et al. 2017. (f) The spectral index of the dust opacity β, the column density 
, and the mass in solar units are estimated considering a temperature of the dust Td ~ 35 K for the starless core MM1a, MM3a, MM9, and for the young sources MM6c and MM11a, while a Td ~ 100 K was used for the hot cores MM4a, MM7 and MM8a. (g) To compute the mass to flux ratio we used the magnetic field values obtained by SF analysis.
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