Table 1.
Overview of the ALMA-IMF protocluster clouds and their evolutionary stage.
| Protocluster | RA (1) | Dec (1) | VLSR(1) | d(1) | Evolutionary | Imaged areas(3) | fBW lines(4) | ||
|---|---|---|---|---|---|---|---|---|---|
| cloud name (1) | [ICRS (J2000)] | [km s−1] | [kpc] | stage (2) | [pc × pc] | B3 | B6 | ||
| A1.3 mm | A3 mm | ||||||||
| W43–MM1 | 18:47:47.00 | −01:54:26.0 | +97 | 5.5 ± 0.4 | Y | 3.1 × 2.3 | 5.1 × 4.0 | 0.64 | 0.55 |
| W43–MM2 | 18:47:36.61 | −02:00:51.1 | +97 | 5.5 ± 0.4 | Y | 2.6 × 2.4 | 5.1 × 4.0 | 0.46 | 0.52 |
| G338.93 | 16:40:34.42 | −45:41:40.6 | −62 | 3.9 ± 1.0 | Y | 1.6 × 1.6 | 2.9 × 2.8 | 0.49 | 0.25 |
| G328.25 | 15:57:59.68 | −53:58:00.2 | −43 | 2.5 ± 0.5 | Y | 1.4 × 1.4 | 2.2 × 1.9 | 0.2 | 0.53 |
| G337.92 | 16:41:10.62 | −47:08:02.9 | −40 | 2.7 ± 0.7 | Y | 1.2 × 1.1 | 2.1 × 2.0 | 0.37 | 0.53 |
| G327.29 | 15:53:08.13 | −54:37:08.6 | −45 | 2.5 ± 0.5 | Y | 1.3 × 1.3 | 1.9 × 1.8 | 0.65 | 0.48 |
| G351.77 | 17:26:42.62 | −36:09:20.5 | −3 | 2.0 ± 0.7 | I | 1.3 × 1.3 | 1.8 × 1.7 | 0.64 | 0.56 |
| G008.67 | 18:06:21.12 | −21:37:16.7 | +37.6 | 3.4 ± 0.3 | I | 2.2 × 1.4 | 3.1 × 2.1 | 0.22 | 0.29 |
| W43-MM3 | 18:47:41.46 | −02:00:27.6 | +97 | 5.5 ± 0.4 | I | 2.7 × 2.4 | 5.1 × 4.0 | 0.13 | 0.08 |
| W51-E | 19:23:44.18 | +14:30:29.5 | +55 | 5.4 ± 0.3 | I | 2.6 × 2.4 | 4.2 × 3.9 | 0.3 | 0.37 |
| G353.41 | 17:30:26.28 | −34:41:49.7 | −17 | 2.0 ± 0.7 | I | 1.3 × 1.3 | 1.8 × 1.7 | 0.14 | 0.08 |
| G010.62 | 18:10:28.84 | −19:55:48.3 | −2 | 4.95 ± 0.5 | E | 2.3 × 2.2 | 3.8 × 3.6 | 0.11 | 0.28 |
| W51-IRS2 | 19:23:39.81 | +14:31:03.5 | +55 | 5.4 ± 0.3 | E | 2.6 × 2.4 | 4.2 × 3.9 | 0.26 | 0.42 |
| G012.80 | 18:14:13.37 | −17:55:45.2 | +37 | 2.4 ± 0.2 | E | 1.5 × 1.5 | 2.2 × 2.1 | 0.12 | 0.16 |
| G333.60 | 16:22:09.36 | −50:05:58.9 | −47 | 4.2 ± 0.7 | E | 2.9 × 2.9 | 3.9 × 3.7 | 0.16 | 0.2 |
Notes.
Protocluster name, central position, and velocity relative to the local standard of rest used for the ALMA-IMF observations. VLSR values are taken from the high-density gas studies by Wienen et al. (2015), Ginsburg et al. (2015) for W51, Nguyen-Luong et al. (2013) for W43, and Immer et al. (2014) for G012.80. The phase centre of W43-MM1 in the pilot study is RA = 18:47:46.50, Dec = − 01:54:29.5. Distances are taken from Motte et al. (2022) and references therein.
Classification of the ALMA-IMF protocluster clouds: Young (Y), Intermediate (I), and Evolved (E). See Sect. 4.1 of Motte et al. (2022).
Physical areas encompassing the combined primary beams of the 1.3 mm and 3 mm mosaics. The released maps cover an area down to the full width at 10% of the maximum of the primary beam response.
This is the fraction of the bandwidth found to contain bright line emission, which was excluded to make the cleanest continuum cubes, i.e. 1 − fBW, cleanest from Table 3 of Ginsburg et al. (2022a). To first order, this fraction highlights the percentage of bandwidth containing bright line emission and illustrates the variation of molecular emission between the regions.
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