by lines; hence, they are most likely outflow knots (see Sect. 4.3). We also corrected the flux density for four additional cores whose emission at 1.3 mm was contaminated by line emission. At this stage, our core catalogue contained 80 sources.

- We constrained the evolutionary stage of these 80 sources in Sect. 5. Based on infrared data, we first found one clear association of our source #24 with a Class I source and one clear association of our source #19 with a methanol maser, and two less clear correlations between cores from our list and H₂O masers. We identified four hot-core candidates using complex organic molecule spectra (Fig. 7) and 20 cores associated with either CO and/or SiO outflows (see Fig. 8 for examples). All four hot-core candidates are associated with outflows, but the Class I source is not, and hence we counted 21 robust protostellar sources. In scenario A, we consider them to be only protostellar (and the 59 others to be prestellar). For 16 cores, though, their location in free-free-contaminated regions made the association with an outflow unclear. In scenario B, we included them in the protostellar sub-sample (for a tally of 37 protostellar and 43 prestellar cores). Our findings on the nature of cores can be found in Fig. 9.

- We then converted the flux densities at 1.3 mm for all of our cores to masses. This conversion depends on dust temperature, which we obtained using the PPMAP procedure (see Fig. 10) and core-scale prescriptions. The resulting CMF built from the complete core sample of W33-Main has a power-law behaviour with a slope slightly steeper than, but consistent with, the Salpeter value ($\alpha = -1.44^{+0.16}_{-0.22}$, see Figs. 11 and 12 in Sect. 6). Once split in prestellar and protostellar sub-samples (see Sect. 7), we found respective values of $\alpha = -1.69^{+0.20}_{-0.31}$ and $\alpha = -1.04^{+0.15}_{-0.31}$ (scenario A; see Fig. 13) and $\alpha = -1.75^{+0.24}_{-0.42}$ and $\alpha = -1.25^{+0.17}_{-0.33}$ (scenario B).

- These results were obtained on small samples and should be treated with caution. However, they are compatible with a 'clump-fed' scenario of star formation in an evolved cloud having already gone through hierarchical infall and where stellar feedback is operating in the form of H II regions probably driven by the most massive stars belonging to the same generation as the cores we detected, and also through energetic photons emitted by massive stars located outside of W33-Main. The masses of protostellar cores are a bit higher than those of the prestellar ones, the proportion of massive protostars is higher than that of the prestellar ones, there are no massive prestellar cores, but some low-mass protostellar ones. The star formation seems to proceed more efficiently in the central region, which could be due to the compression fronts generated by the H II regions. The cores' masses are low in the whole observed field, which could be due to energetic photons emitted by the stars driving the H II regions and by massive stars outside W33-Main.

Our results call for investigations in a statistical sample of evolved regions. Indeed, our results differ from those found in less evolved, young, star-forming regions by the ALMA-IMF programme. If confirmed, the CMF of massive protoclusters could initially be top-heavy, but steepen to reconcile with the Salpeter IMF due to i) feedback effects exerted by stars (either from previous generations or the fastest evolving ones from the same generation) on the cloud, and/or ii) dynamical relaxation of the region leading to the formation of less dense filaments harbouring the new cores, and/or iii) the transformation of the most massive cores of the same generation in massive stars having already occurred. Our results perhaps also call for dedicated

investigations on peculiar sources found in our sample such as 'uncertain' sources, which are contaminated cores associated with outflows or located at the centre of the most prominent H II region.

**Acknowledgements.** We are grateful to the anonymous referee for the various suggestions that resulted in a significant improvement of this article. This article makes use of the ALMA data ADS/JAO.ALMA#2017.1.01355.L. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The project leading to this publication has received support from ORP, that is funded by the European Union's Horizon 2020 research and innovation programme under grant agreement No 101004719 [ORP]. F.M., N.C., and F.L. also acknowledge support from the European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130), from the French Agence Nationale de la Recherche (ANR) through the project COSMHIC (ANR-20-CE31-0009), and the French Programme National de Physique Stellaire and Physique et Chimie du Milieu Interstellaire (PNPS and PCMI) of CNRS/INSU (with INC/INP/IN2P3). R.G.M. and D.D.G. acknowledge support from UNAM-PAPIIT project IN108822, and from CONACyT Ciencia de Frontera project ID: 86372. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This publication also uses data from the ATLASGAL project, a collaboration between the Max-Planck-Gesellschaft, the European stern Observatory (ESO) and the Universidad de Chile. It includes projects E-181.C-0885, E-078.F-9040(A), M-079.C-9501(A), M-081.C-9501(A) plus Chilean data. This work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. PS was partially supported by a Grant-in-Aid for Scientific Research (KAKENHI Number JP22H01271 and JP23H01221) of JSPS. Melisse Bonfand is a postdoctoral fellow in the University of Virginia's VICO collaboration and is funded by grants from the NASA Astrophysics Theory Program (grant number 80NSSC18K0558) and the NSF Astronomy & Astrophysics program (grant number 2206516). A.G. acknowledges support from the NSF via grants AST 2008101 and CAREER 2142300. A.S. gratefully acknowledges support by the Fondecyt Regular (project code 1220610), and ANID BASAL projects ACE210002 and FB210003.

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# Appendix A: Search for class I, II, and masers

Using archival observations in the mid-infrared and mid-near-infrared ranges, we attempted to identify if low-mass objects at advanced stages of evolution (class I, II and older) are present in this region, and if so, to assess their evolutionary stage based on their infrared fluxes.

<figure><img src="image_17.png" /><figcaption>**Fig. A.1.** IRAC 3.6 µm map of W33-Main field observed by ALMA-IMF, reprojected on the ALMA 1.3 mm *bsens* dataset, with the cores from the *getsf* filtered catalogue in black ellipses. *Panel a:* In coloured markers are the infrared sources identified using 2MASS (cyan), WISE (white), and *Spitzer*/IRAC (Messineo et al. 2015) (other colors). *Panel b:* In coloured markers are the infrared sources identified using GLIMPSE.</figcaption></figure>

## A.1. 2MASS and WISE all-sky surveys

The W33 complex was fully mapped by both the 2MASS (Skrutskie et al. 2006) and WISE (Wright et al. 2010) all-sky surveys. 2MASS operates between 1.235 µm and 2.159 µm, and WISE between 3.4 µm and 22 µm. A total of 117 point sources in the 2MASS All-Sky Point Source Catalogue and 19 point sources in the AllWISE Source Catalogue were found in the W33-Main field observed by the ALMA-IMF Large

Programme. In order to reject false positives, we applied several selection criteria to these primary point source catalogues. Our method required simultaneous detections in the $W_1$, $W_2$ bands of WISE or in the J, H, and K bands of 2MASS, and we then only selected the sources with a signal-to-noise ratio greater than two in these bands. After this selection, 32 point sources remained for the 2MASS catalogue and ten remained for the WISE one.

We then applied colour-colour criteria to these remaining point sources to select young stellar object candidates. For 2MASS objects, we compared the relative flux in the J, H, and K bands. We used the empirical colour criteria introduced by Xu et al. (2011). This set of conditions between the fluxes in various channels allowed us to distinguish cool giants, normally reddened stars, Classical T Tauri stars, He Ae/Be stars, and in general, infrared excess sources, including young stellar objects that do not fall into any of these categories. Similarly, we used a colour-colour criterion (Koenig & Leisawitz 2014) to characterise the point sources from the flux measurements of bands $W_1$, $W_2$, and $W_3$ of WISE. With these, we distinguished two evolutionary stages: Class I and Class II protostars, defined by their respective infrared excess. After the colour-colour filtering of the catalogues, the total amount of remaining point sources is three (one CTTS and two HAeBe) for 2MASS and one Class I for WISE within the field observed by the ALMA-IMF programme. We also included the point sources catalogued by Messineo et al. (2015) in this study: one star cluster, one O-type star, two water masers, and one methanol maser.

Our results can be seen in Fig. A.1a. We found a clear association between our prestellar core #24 and a Class I protostar detected in the WISE catalogue. For this core, we retained the protostellar classification. We also found a possible association between our protostellar core #19 and a CH$_3$OH maser, and two other potential associations between several of our sources with the two water masers. We note, however, that for these water masers, the association is more ambiguous than for the methanol maser: one is located within the H II region '2-3' near cores #27 and #18, and the other one in a H II region surroundings between region '2-3' and region '4', near cores #71 and #79.

## A.2. GLIMPSE Galactic plane survey

The W33 complex was also fully mapped by the GLIMPSE (Churchwell et al. 2009) Galactic plane survey. GLIMPSE I imaged at wavelengths 3.6, 4.5, 5.8, and 8.0 µm using the IRAC instrument (Infrared Array Camera) of the *Spitzer* telescope. A total of 210 point sources in the GLIMPSE I Catalogue were found in the W33-Main field observed by the ALMA-IMF Large programme. In order to reject false positives, we applied several selection criteria to this primary catalogue of point sources: our method required simultaneous detections in all IRAC bands, and we then only selected the sources with a signal-to-noise ratio greater than two in these bands. After this selection, 46 point sources remained in the GLIMPSE catalogue.

We then applied colour-colour criteria to these remaining point sources to select young stellar object candidates. We compared the relative flux in all the four bands. We used the colour-colour criteria of Allen et al. (2004). This set of conditions between bands [3.6]-[4.5] and [5.8]-[8.0] allowed us to distinguish between three evolutionary stages: Class I, Class II, and more evolved protostars (CTTS and HAeBe), defined
# Appendix A: Search for class I, II, and masers

Using archival observations in the mid-infrared and mid-near-infrared ranges, we attempted to identify if low-mass objects at advanced stages of evolution (class I, II and older) are present in this region, and if so, to assess their evolutionary stage based on their infrared fluxes.

<figure><img src="image_16.png" /><figcaption>**Fig. A.1.** IRAC 3.6 µm map of W33-Main field observed by ALMA-IMF, reprojected on the ALMA 1.3 mm *bsens* dataset, with the cores from the *getsf* filtered catalogue in black ellipses. *Panel a:* In coloured markers are the infrared sources identified using 2MASS (cyan), WISE (white), and *Spitzer*/IRAC (Messineo et al. 2015) (other colors). *Panel b:* In coloured markers are the infrared sources identified using GLIMPSE.</figcaption></figure>

## A.1. 2MASS and WISE all-sky surveys

The W33 complex was fully mapped by both the 2MASS (Skrutskie et al. 2006) and WISE (Wright et al. 2010) all-sky surveys. 2MASS operates between 1.235 µm and 2.159 µm, and WISE between 3.4 µm and 22 µm. A total of 117 point sources in the 2MASS All-Sky Point Source Catalogue and 19 point sources in the AllWISE Source Catalogue were found in the W33-Main field observed by the ALMA-IMF Large

Programme. In order to reject false positives, we applied several selection criteria to these primary point source catalogues. Our method required simultaneous detections in the $W_1$, $W_2$ bands of WISE or in the J, H, and K bands of 2MASS, and we then only selected the sources with a signal-to-noise ratio greater than two in these bands. After this selection, 32 point sources remained for the 2MASS catalogue and ten remained for the WISE one.

We then applied colour-colour criteria to these remaining point sources to select young stellar object candidates. For 2MASS objects, we compared the relative flux in the J, H, and K bands. We used the empirical colour criteria introduced by Xu et al. (2011). This set of conditions between the fluxes in various channels allowed us to distinguish cool giants, normally reddened stars, Classical T Tauri stars, He Ae/Be stars, and in general, infrared excess sources, including young stellar objects that do not fall into any of these categories. Similarly, we used a colour-colour criterion (Koenig & Leisawitz 2014) to characterise the point sources from the flux measurements of bands $W_1$, $W_2$, and $W_3$ of WISE. With these, we distinguished two evolutionary stages: Class I and Class II protostars, defined by their respective infrared excess. After the colour-colour filtering of the catalogues, the total amount of remaining point sources is three (one CTTS and two HAeBe) for 2MASS and one Class I for WISE within the field observed by the ALMA-IMF programme. We also included the point sources catalogued by Messineo et al. (2015) in this study: one star cluster, one O-type star, two water masers, and one methanol maser.

Our results can be seen in Fig. A.1a. We found a clear association between our prestellar core #24 and a Class I protostar detected in the WISE catalogue. For this core, we retained the protostellar classification. We also found a possible association between our protostellar core #19 and a CH$_3$OH maser, and two other potential associations between several of our sources with the two water masers. We note, however, that for these water masers, the association is more ambiguous than for the methanol maser: one is located within the H II region ‘2-3’ near cores #27 and #18, and the other one in a H II region surroundings between region ‘2-3’ and region ‘4’, near cores #71 and #79.

## A.2. GLIMPSE Galactic plane survey

The W33 complex was also fully mapped by the GLIMPSE (Churchwell et al. 2009) Galactic plane survey. GLIMPSE I imaged at wavelengths 3.6, 4.5, 5.8, and 8.0 µm using the IRAC instrument (Infrared Array Camera) of the *Spitzer* telescope. A total of 210 point sources in the GLIMPSE I Catalogue were found in the W33-Main field observed by the ALMA-IMF Large programme. In order to reject false positives, we applied several selection criteria to this primary catalogue of point sources: our method required simultaneous detections in all IRAC bands, and we then only selected the sources with a signal-to-noise ratio greater than two in these bands. After this selection, 46 point sources remained in the GLIMPSE catalogue.

We then applied colour-colour criteria to these remaining point sources to select young stellar object candidates. We compared the relative flux in all the four bands. We used the colour-colour criteria of Allen et al. (2004). This set of conditions between bands [3.6]-[4.5] and [5.8]-[8.0] allowed us to distinguish between three evolutionary stages: Class I, Class II, and more evolved protostars (CTTS and HAeBe), defined
by their respective infrared excess. After this colour-colour filtering of the catalogue, six Class I, one Class II, and seven more evolved objects were found within the field observed by the ALMA-IMF program.

These results can be seen in Fig. A.1b. We found one Class I protostar not associated with any of our cores, and one source that could be classified either as a Class I or a Class II protostar, not associated with any of our cores, but whose position correlates with the Oe star classified by Messineo et al. (2015)<fnref n="10" />. We found four CTTS or HAeBe stars with no association with any of our cores, and three of them with a potential but unclear association with our cores: two between prestellar cores (one between #60 and #89 and one between #32 and #16), and one between the two protostellar cores #84 and #43. We did not find any association between point sources identified using the 2MASS and WISE catalogues on the one hand, and the GLIMPSE catalogue on the other hand.

## Appendix B: Complementary figure and table

We estimated a 90% global completeness level of 1.0 ± 0.2 M<sub>☉</sub> for the *getsf* catalogue based on the method presented in Sect. 4.1. Fig. B.1 details how it was reached in W33-Main.

<figure><img src="image_18.png" /></figure>

**Fig. B.1.** Completeness level of ~800 synthetic cores added on background image of W33-Main. The core content is 90% complete down to 1.0 ± 0.2 M<sub>☉</sub> for the *getsf* catalogue. The error bars represent the ±1σ uncertainties for mass estimates across each bin (x-axis) and total cores retrieved per bin (y-axis). Data points were interpolated using the piecewise cubic hermite interpolating polynomial method. Blue points represent the full sample of cores detected by *getsf*

<footnote n="10">¹⁰ The fact that this source can simultaneously be classified a Class I or II protostar or as a Oe star illustrates the uncertainty of this kind of search.</footnote>
by their respective infrared excess. After this colour-colour filtering of the catalogue, six Class I, one Class II, and seven more evolved objects were found within the field observed by the ALMA-IMF program.

These results can be seen in Fig. A.1b. We found one Class I protostar not associated with any of our cores, and one source that could be classified either as a Class I or a Class II protostar, not associated with any of our cores, but whose position correlates with the Oe star classified by Messineo et al. (2015)<fnref n="10" />. We found four CTTS or HAeBe stars with no association with any of our cores, and three of them with a potential but unclear association with our cores: two between prestellar cores (one between #60 and #89 and one between #32 and #16), and one between the two protostellar cores #84 and #43. We did not find any association between point sources identified using the 2MASS and WISE catalogues on the one hand, and the GLIMPSE catalogue on the other hand.

## Appendix B: Complementary figure and table

We estimated a 90% global completeness level of 1.0 ± 0.2 M<sub>☉</sub> for the *getsf* catalogue based on the method presented in Sect. 4.1. Fig. B.1 details how it was reached in W33-Main.

<figure><img src="image_17.png" /></figure>

**Fig. B.1.** Completeness level of ~800 synthetic cores added on background image of W33-Main. The core content is 90% complete down to 1.0 ± 0.2 M<sub>☉</sub> for the *getsf* catalogue. The error bars represent the ±1σ uncertainties for mass estimates across each bin (x-axis) and total cores retrieved per bin (y-axis). Data points were interpolated using the piecewise cubic hermite interpolating polynomial method. Blue points represent the full sample of cores detected by *getsf*.

<footnote n="10">¹⁰ The fact that this source can simultaneously be classified a Class I or II protostar or as a Oe star illustrates the uncertainty of this kind of search.</footnote>
<table><caption>Table B.1. Table of properties of 94 sources extracted by *getsf* in W33-Main using the 1.3 mm *bsens* continuum map ('filtered' catalogue).</caption><thead><tr><th>n</th><th>R.A. [J2000]<br>hms</th><th>Dec. [J2000]<br>°′′</th><th>a<sub>1.3 mm</sub><br>b<sub>1.3 mm</sub><br>[pix × pix]</th><th>PA<sub>1.3 mm</sub><br>[deg]</th><th>S<sup>peak</sup><sub>1.3 mm</sub><br>[mJy beam<sup>-1</sup>]</th><th>S<sup>int</sup><sub>1.3 mm</sub><br>[mJy]</th><th>a<sub>3 mm</sub><br>b<sub>3 mm</sub><br>[pix × pix]</th><th>PA<sub>3 mm</sub><br>[deg]</th><th>S<sup>peak</sup><sub>3 mm</sub><br>[mJy beam<sup>-1</sup>]</th><th>S<sup>int</sup><sub>3 mm</sub><br>[mJy]</th><th>Gex2D<br>(a)</th><th>tag</th><th>Nature<sup>(b)</sup></th></tr></thead><tbody><tr><td>1</td><td>18:14:11.84</td><td>-17:55:32.45</td><td>7.5 × 5.5</td><td>64</td><td>195.20 ± 10.51</td><td>306.80 ± 10.20</td><td>10.3 × 8.6</td><td>60</td><td>24.32 ± 1.24</td><td>28.77 ± 0.96</td><td>**</td><td>Hot core</td><td></td></tr><tr><td>2</td><td>18:14:13.77</td><td>-17:55:20.99</td><td>9.1 × 6.6</td><td>46</td><td>112.30 ± 4.02</td><td>272.20 ± 5.96</td><td>9.4 × 8.2</td><td>11</td><td>11.41 ± 4.50</td><td>10.63 ± 3.47</td><td>**</td><td>Free-free, hot core</td><td></td></tr><tr><td>3</td><td>18:14:10.66</td><td>-17:56:15.12</td><td>7.0 × 4.6</td><td>77</td><td>35.81 ± 1.01</td><td>45.70 ± 1.05</td><td>9.2 × 7.9</td><td>74</td><td>3.64 ± 0.23</td><td>3.87 ± 0.20</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>4</td><td>18:14:11.56</td><td>-17:56:45.02</td><td>7.6 × 5.1</td><td>89</td><td>46.08 ± 1.37</td><td>65.64 ± 1.33</td><td>10.0 × 7.8</td><td>79</td><td>7.15 ± 0.31</td><td>8.03 ± 0.25</td><td>**</td><td></td><td></td></tr><tr><td>5</td><td>18:14:12.76</td><td>-17:55:14.86</td><td>7.9 × 5.7</td><td>64</td><td>36.54 ± 1.31</td><td>69.93 ± 1.64</td><td>14.0 × 13.1</td><td>110</td><td>4.66 ± 1.55</td><td>9.31 ± 1.35</td><td>**</td><td></td><td></td></tr><tr><td>6</td><td>18:14:13.38</td><td>-17:54:54.46</td><td>6.8 × 5.9</td><td>52</td><td>19.32 ± 1.02</td><td>29.58 ± 1.06</td><td>10.3 × 8.2</td><td>42</td><td>3.42 ± 0.35</td><td>4.26 ± 0.32</td><td>**</td><td></td><td></td></tr><tr><td>7</td><td>18:14:13.14</td><td>-17:55:40.39</td><td>8.2 × 6.4</td><td>70</td><td>93.65 ± 16.36</td><td>178.50 ± 16.87</td><td>10.3 × 10.0</td><td>2</td><td>16.26 ± 14.10</td><td>22.94 ± 10.87</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>8</td><td>18:14:10.68</td><td>-17:55:49.13</td><td>8.2 × 6.9</td><td>68</td><td>19.37 ± 1.29</td><td>40.63 ± 1.51</td><td>10.8 × 10.3</td><td>48</td><td>2.38 ± 0.46</td><td>3.24 ± 0.35</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>9</td><td>18:14:13.01</td><td>-17:54:50.98</td><td>7.4 × 4.4</td><td>76</td><td>18.35 ± 0.76</td><td>21.25 ± 0.66</td><td>9.5 × 7.4</td><td>87</td><td>2.38 ± 0.26</td><td>2.96 ± 0.24</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>11</td><td>18:14:12.64</td><td>-17:55:42.90</td><td>7.2 × 5.1</td><td>67</td><td>21.41 ± 1.27</td><td>29.40 ± 1.14</td><td>41.37 ± 2.19</td><td>–</td><td>≤ 1.631</td><td>≤ 1.631</td><td>**</td><td>Free-free, outflows</td><td></td></tr><tr><td>12</td><td>18:14:13.48</td><td>-17:55:16.81</td><td>7.3 × 6.5</td><td>68</td><td>24.29 ± 2.25</td><td>–</td><td>–</td><td>–</td><td>≤ 0.723</td><td>≤ 0.723</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>13</td><td>18:14:11.64</td><td>-17:55:34.22</td><td>10.9 × 6.1</td><td>93</td><td>63.11 ± 10.08</td><td>116.70 ± 10.21</td><td>12.6 × 9.3</td><td>91</td><td>9.12 ± 1.18</td><td>12.20 ± 0.95</td><td>**</td><td>Hot core</td><td></td></tr><tr><td>14</td><td>18:14:11.62</td><td>-17:56:28.51</td><td>9.3 × 7.2</td><td>22</td><td>7.27 ± 0.42</td><td>19.87 ± 0.58</td><td>15.3 × 14.6</td><td>86</td><td>0.94 ± 0.19</td><td>2.94 ± 0.22</td><td>**</td><td></td><td></td></tr><tr><td>15</td><td>18:14:14.29</td><td>-17:55:13.31</td><td>14.7 × 11.8</td><td>120</td><td>22.59 ± 6.05</td><td>112.80 ± 7.74</td><td>14.8 × 11.3</td><td>120</td><td>53.37 ± 17.81</td><td>108.60 ± 15.19</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>16</td><td>18:14:15.86</td><td>-17:55:24.33</td><td>7.3 × 5.1</td><td>61</td><td>15.07 ± 1.25</td><td>20.55 ± 1.04</td><td>10.9 × 8.5</td><td>87</td><td>2.86 ± 0.41</td><td>4.16 ± 0.41</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>17</td><td>18:14:12.80</td><td>-17:55:40.76</td><td>11.6 × 8.6</td><td>92</td><td>7.75 ± 3.60</td><td>22.37 ± 3.90</td><td>–</td><td>–</td><td>≤ 1.398</td><td>≤ 1.400</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>18</td><td>18:14:14.06</td><td>-17:55:43.19</td><td>8.1 × 6.2</td><td>38</td><td>25.02 ± 11.94</td><td>39.59 ± 9.22</td><td>13.6 × 10.0</td><td>39</td><td>71.26 ± 32.10</td><td>105.50 ± 24.77</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>19</td><td>18:14:11.29</td><td>-17:56:00.26</td><td>8.1 × 6.7</td><td>46</td><td>8.36 ± 0.86</td><td>17.54 ± 0.94</td><td>13.9 × 13.1</td><td>20</td><td>0.99 ± 0.30</td><td>2.26 ± 0.30</td><td>**</td><td>CH<sub>3</sub>OH maser</td><td></td></tr><tr><td>20</td><td>18:14:14.05</td><td>-17:55:15.15</td><td>26.0 × 20.0</td><td>49</td><td>10.24 ± 3.71</td><td>139.70 ± 8.10</td><td>17.3 × 12.9</td><td>17</td><td>30.22 ± 14.69</td><td>77.31 ± 15.81</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>21</td><td>18:14:13.95</td><td>-17:55:58.44</td><td>12.3 × 10.9</td><td>127</td><td>13.27 ± 2.48</td><td>71.46 ± 4.04</td><td>17.3 × 14.1</td><td>124</td><td>25.97 ± 8.43</td><td>81.02 ± 8.76</td><td>**</td><td>Free-free</td><td></td></tr><tr><td>22</td><td>18:14:16.57</td><td>-17:55:29.00</td><td>8.8 × 6.2</td><td>83</td><td>9.77 ± 0.85</td><td>20.98 ± 0.99</td><td>16.0 × 14.3</td><td>138</td><td>1.66 ± 0.33</td><td>4.29 ± 0.33</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>23</td><td>18:14:11.14</td><td>-17:55:43.07</td><td>8.6 × 6.5</td><td>62</td><td>20.09 ± 4.38</td><td>38.03 ± 4.25</td><td>11.1 × 9.3</td><td>0</td><td>3.42 ± 0.57</td><td>5.30 ± 0.57</td><td>**</td><td>CO-contaminated</td><td></td></tr><tr><td>24</td><td>18:14:10.09</td><td>-17:55:57.82</td><td>10.6 × 6.6</td><td>57</td><td>17.04 ± 2.18</td><td>40.28 ± 2.20</td><td>12.3 × 8.8</td><td>55</td><td>3.32 ± 0.52</td><td>4.51 ± 0.41</td><td>**</td><td>Class I</td><td></td></tr><tr><td>25</td><td>18:14:16.25</td><td>-17:55:13.82</td><td>9.7 × 1.3</td><td>153</td><td>21.06 ± 1.08</td><td>21.0 ± 1.08</td><td>13.8 × 11.2</td><td>0</td><td>0.50 ± 0.34</td><td>0.59 ± 0.35</td><td>**</td><td></td><td></td></tr><tr><td>26</td><td>18:14:13.46</td><td>-17:55:42.02</td><td>10.2 × 7.7</td><td>56</td><td>60.35 ± 12.55</td><td>113.00 ± 17.71</td><td>13.7 × 12.1</td><td>68</td><td>59.68 ± 43.04</td><td>116.40 ± 33.17</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>27</td><td>18:14:14.10</td><td>-17:55:39.64</td><td>9.1 × 6.5</td><td>83</td><td>52.79 ± 18.23</td><td>113.00 ± 17.71</td><td>–</td><td>–</td><td>≤ 31.000</td><td>≤ 23.880</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>28</td><td>18:14:13.78</td><td>-17:55:41.33</td><td>7.9 × 4.9</td><td>57</td><td>41.09 ± 17.04</td><td>53.23 ± 13.31</td><td>–</td><td>–</td><td>≤ 27.000</td><td>≤ 27.040</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>29</td><td>18:14:12.41</td><td>-17:55:08.30</td><td>10.1 × 7.9</td><td>96</td><td>7.63 ± 1.23</td><td>22.17 ± 1.79</td><td>–</td><td>–</td><td>≤ 0.361</td><td>≤ 0.435</td><td>**</td><td>CO-contaminated</td><td></td></tr><tr><td>30</td><td>18:14:11.34</td><td>-17:55:19.55</td><td>10.1 × 9.0</td><td>89</td><td>6.18 ± 0.61</td><td>19.81 ± 0.71</td><td>16.7 × 14.3</td><td>77</td><td>0.70 ± 0.20</td><td>1.98 ± 0.20</td><td>**</td><td></td><td></td></tr><tr><td>31</td><td>18:14:17.15</td><td>-17:55:29.83</td><td>6.4 × 4.2</td><td>70</td><td>10.34 ± 0.85</td><td>10.64 ± 0.69</td><td>11.1 × 9.1</td><td>38</td><td>0.81 ± 0.38</td><td>0.97 ± 0.38</td><td>**</td><td></td><td></td></tr><tr><td>32</td><td>18:14:15.96</td><td>-17:55:22.22</td><td>9.3 × 6.6</td><td>59</td><td>10.71 ± 1.31</td><td>22.53 ± 1.28</td><td>13.1 × 11.4</td><td>111</td><td>2.09 ± 0.50</td><td>4.41 ± 0.50</td><td>**</td><td></td><td></td></tr><tr><td>33</td><td>18:14:13.48</td><td>-17:56:05.49</td><td>9.4 × 8.6</td><td>10</td><td>7.90 ± 1.26</td><td>22.44 ± 1.58</td><td>–</td><td>–</td><td>≤ 0.535</td><td>≤ 0.558</td><td>**</td><td></td><td></td></tr><tr><td>34</td><td>18:14:16.55</td><td>-17:56:20.48</td><td>10.2 × 5.7</td><td>66</td><td>5.08 ± 0.40</td><td>11.26 ± 0.46</td><td>–</td><td>–</td><td>≤ 0.024</td><td>≤ 0.025</td><td>**</td><td></td><td></td></tr><tr><td>35</td><td>18:14:14.92</td><td>-17:55:48.80</td><td>23.7 × 15.2</td><td>122</td><td>11.15 ± 3.32</td><td>112.20 ± 7.20</td><td>21.7 × 13.3</td><td>117</td><td>26.18 ± 14.58</td><td>97.64 ± 20.25</td><td>**</td><td>Free-free, outflows</td><td></td></tr><tr><td>36</td><td>18:14:13.67</td><td>-17:55:23.94</td><td>7.1 × 5.4</td><td>39</td><td>20.96 ± 4.92</td><td>28.47 ± 3.84</td><td>–</td><td>–</td><td>≤ 1.842</td><td>≤ 1.843</td><td>**</td><td></td><td></td></tr><tr><td>37</td><td>18:14:15.88</td><td>-17:55:32.39</td><td>8.9 × 6.8</td><td>56</td><td>5.97 ± 0.73</td><td>12.58 ± 0.79</td><td>–</td><td>–</td><td>≤ 0.409</td><td>≤ 0.410</td><td>**</td><td></td><td></td></tr><tr><td>38</td><td>18:14:12.28</td><td>-17:55:30.87</td><td>12.6 × 7.0</td><td>39</td><td>3.33 ± 0.99</td><td>3.33 ± 0.99</td><td>–</td><td>–</td><td>≤ 0.191</td><td>≤ 0.192</td><td>**</td><td></td><td></td></tr><tr><td>39</td><td>18:14:13.83</td><td>-17:55:52.23</td><td>8.8 × 7.7</td><td>41</td><td>53.00 ± 5.95</td><td>16.6 × 12.6</td><td>–</td><td>–</td><td>20.90 ± 8.34</td><td>54.15 ± 8.36</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>40</td><td>18:14:13.66</td><td>-17:55:26.01</td><td>9.0 × 6.8</td><td>59</td><td>30.67 ± 2.96</td><td>–</td><td>–</td><td>–</td><td>≤ 2.736</td><td>≤ 2.740</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>41</td><td>18:14:11.00</td><td>-17:55:42.02</td><td>6.8 × 5.7</td><td>80</td><td>16.11 ± 3.40</td><td>22.65 ± 3.49</td><td>14.9 × 12.4</td><td>8</td><td>3.30 ± 0.50</td><td>8.08 ± 0.51</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>42</td><td>18:14:14.83</td><td>-17:55:32.25</td><td>12.9 × 8.1</td><td>89</td><td>16.64 ± 4.31</td><td>13.65 ± 2.70</td><td>–</td><td>–</td><td>≤ 0.806</td><td>≤ 0.972</td><td>**</td><td>Free-free</td><td></td></tr><tr><td>43</td><td>18:14:11.16</td><td>-17:55:39.70</td><td>9.0 × 7.4</td><td>40</td><td>5.06 ± 1.43</td><td>31.21 ± 3.85</td><td>14.1 × 12.1</td><td>21</td><td>3.26 ± 0.56</td><td>7.47 ± 0.56</td><td>**</td><td>Outflows</td><td></td></tr><tr><td>44</td><td>18:14:14.24</td><td>-17:55:15.40</td><td>9.8 × 7.6</td><td>59</td><td>14.11 ± 4.09</td><td>15.41 ± 4.42</td><td>11.7 × 8.7</td><td>54</td><td>26.10 ± 6.50</td><td>36.32 ± 6.53</td><td>**</td><td>Free-free</td><td></td></tr><tr><td>45</td><td>18:14:14.76</td><td>-17:55:45.88</td><td>12.0 × 8.5</td><td>117</td><td>7.15 ± 4.55</td><td>66.27 ± 5.59</td><td>17.5 × 13.5</td><td>116</td><td>39.16 ± 17.92</td><td>112.10 ± 17.95</td><td>**</td><td>Free-free</td><td></td></tr><tr><td>46</td><td>18:14:13.96</td><td>-17:55:31.07</td><td>10.4 × 6.9</td><td>27</td><td>20.82 ± 4.60</td><td>53.37 ± 4.99</td><td>–</td><td>–</td><td>≤ 2.524</td><td>≤ 2.530</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr><tr><td>47</td><td>18:14:13.77</td><td>-17:55:31.17</td><td>7.7 × 5.9</td><td>79</td><td>8.40 ± 3.35</td><td>12.45 ± 2.92</td><td>11.4 × 10.4</td><td>95</td><td>22.61 ± 5.02</td><td>34.81 ± 3.87</td><td>**</td><td>Free-free</td><td></td></tr><tr><td>48</td><td>18:14:14.39</td><td>-17:55:29.23</td><td>11.3 × 7.9</td><td>43</td><td>5.80 ± 1.74</td><td>15.06 ± 2.04</td><td>–</td><td>–</td><td>≤ 1.431</td><td>≤ 1.435</td><td>**</td><td>Free-free, outflow ?</td><td></td></tr></tbody></table>
<table><caption>Table B.1. Table of properties of 94 sources extracted by *getsf* in W33-Main using the 1.3 mm *bsens* continuum map ('filtered' catalogue).</caption><thead><tr><th>n</th><th>R.A. [J2000]<br>hms</th><th>Dec. [J2000]<br>°′′</th><th>a<sub>1.3 mm</sub><br>b<sub>1.3 mm</sub><br>[pix × pix]</th><th>PA<sub>1.3 mm</sub><br>[deg]</th><th>S<sup>peak</sup><sub>1.3 mm</sub><br>[mJy beam<sup>-1</sup>]</th><th>S<sup>int</sup><sub>1.3 mm</sub><br>[mJy]</th><th>a<sub>3 mm</sub><br>b<sub>3 mm</sub><br>[pix × pix]</th><th>PA<sub>3 mm</sub><br>[deg]</th><th>S<sup>peak</sup><sub>3 mm</sub><br>[mJy beam<sup>-1</sup>]</th><th>S<sup>int</sup><sub>3 mm</sub><br>[mJy]</th><th>Gex2D<br>(a)<br>tag</th><th>Nature <sup>(b)</sup></th></tr></thead><tbody><tr><td>1</td><td>18:14:11.84</td><td>-17:55:32.45</td><td>7.5 × 5.5</td><td>64</td><td>195.20 ± 10.51</td><td>306.80 ± 10.20</td><td>10.3 × 8.6</td><td>60</td><td>24.32 ± 1.24</td><td>28.77 ± 0.96</td><td>**</td><td>Hot core</td></tr><tr><td>2</td><td>18:14:13.77</td><td>-17:55:20.99</td><td>9.1 × 6.6</td><td>46</td><td>112.30 ± 4.02</td><td>272.20 ± 5.96</td><td>9.4 × 8.2</td><td>11</td><td>11.41 ± 4.50</td><td>10.63 ± 3.47</td><td>**</td><td>Free-free, hot core</td></tr><tr><td>3</td><td>18:14:10.66</td><td>-17:56:15.12</td><td>7.0 × 4.6</td><td>77</td><td>35.81 ± 1.01</td><td>45.70 ± 1.05</td><td>9.2 × 7.9</td><td>74</td><td>3.64 ± 0.23</td><td>3.87 ± 0.20</td><td>**</td><td>Outflows</td></tr><tr><td>4</td><td>18:14:11.56</td><td>-17:56:45.02</td><td>7.9 × 5.7</td><td>89</td><td>46.08 ± 1.37</td><td>65.64 ± 1.33</td><td>10.0 × 7.8</td><td>79</td><td>7.15 ± 0.31</td><td>8.03 ± 0.25</td><td>**</td><td></td></tr><tr><td>5</td><td>18:14:12.76</td><td>-17:55:14.86</td><td>7.9 × 5.7</td><td>64</td><td>36.54 ± 1.31</td><td>69.93 ± 1.64</td><td>14.0 × 13.1</td><td>110</td><td>4.66 ± 1.55</td><td>9.31 ± 1.35</td><td>**</td><td></td></tr><tr><td>6</td><td>18:14:13.38</td><td>-17:54:54.46</td><td>6.8 × 5.9</td><td>52</td><td>19.32 ± 1.02</td><td>29.58 ± 1.06</td><td>10.3 × 8.2</td><td>42</td><td>3.42 ± 0.35</td><td>4.26 ± 0.32</td><td>**</td><td>Outflows</td></tr><tr><td>7</td><td>18:14:13.14</td><td>-17:55:40.39</td><td>8.2 × 6.4</td><td>70</td><td>93.65 ± 16.36</td><td>178.50 ± 16.87</td><td>10.3 × 10.0</td><td>2</td><td>16.26 ± 14.10</td><td>22.94 ± 10.87</td><td>**</td><td>Free-free, hot core</td></tr><tr><td>8</td><td>18:14:10.68</td><td>-17:55:49.13</td><td>8.2 × 6.9</td><td>68</td><td>19.37 ± 1.29</td><td>40.63 ± 1.51</td><td>10.8 × 10.3</td><td>48</td><td>2.38 ± 0.46</td><td>3.24 ± 0.35</td><td>**</td><td>Outflows</td></tr><tr><td>9</td><td>18:14:13.01</td><td>-17:54:50.98</td><td>7.4 × 4.4</td><td>76</td><td>18.35 ± 0.76</td><td>21.25 ± 0.66</td><td>9.5 × 7.4</td><td>87</td><td>2.38 ± 0.26</td><td>2.96 ± 0.24</td><td>**</td><td>Outflows</td></tr><tr><td>11</td><td>18:14:12.64</td><td>-17:55:42.90</td><td>7.2 × 5.1</td><td>67</td><td>21.41 ± 1.27</td><td>29.40 ± 1.14</td><td>41.37 ± 2.19</td><td>–</td><td>≤ 1.631</td><td>≤ 1.631</td><td>**</td><td>Free-free, outflows</td></tr><tr><td>12</td><td>18:14:13.48</td><td>-17:55:16.81</td><td>7.3 × 6.5</td><td>68</td><td>24.29 ± 2.25</td><td>–</td><td>–</td><td>–</td><td>≤ 0.723</td><td>≤ 0.723</td><td>**</td><td>Outflows</td></tr><tr><td>13</td><td>18:14:11.64</td><td>-17:55:34.22</td><td>10.9 × 6.1</td><td>93</td><td>63.11 ± 10.08</td><td>116.70 ± 10.21</td><td>12.6 × 9.3</td><td>91</td><td>9.12 ± 1.18</td><td>12.20 ± 0.95</td><td>**</td><td>Hot core</td></tr><tr><td>14</td><td>18:14:11.62</td><td>-17:56:28.51</td><td>9.3 × 7.2</td><td>22</td><td>7.27 ± 0.42</td><td>19.87 ± 0.58</td><td>15.3 × 14.6</td><td>86</td><td>0.94 ± 0.19</td><td>2.94 ± 0.22</td><td>**</td><td></td></tr><tr><td>15</td><td>18:14:14.29</td><td>-17:55:13.31</td><td>14.7 × 11.8</td><td>120</td><td>22.59 ± 6.05</td><td>112.80 ± 7.74</td><td>14.8 × 11.3</td><td>120</td><td>53.37 ± 17.81</td><td>108.60 ± 15.19</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>16</td><td>18:14:15.86</td><td>-17:55:24.33</td><td>7.3 × 5.1</td><td>61</td><td>15.07 ± 1.25</td><td>20.55 ± 1.04</td><td>10.9 × 8.5</td><td>87</td><td>2.86 ± 0.41</td><td>4.16 ± 0.41</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>17</td><td>18:14:12.80</td><td>-17:55:40.76</td><td>11.6 × 8.6</td><td>92</td><td>7.75 ± 3.60</td><td>22.37 ± 3.90</td><td>–</td><td>–</td><td>≤ 1.398</td><td>≤ 1.400</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>18</td><td>18:14:14.06</td><td>-17:55:43.19</td><td>8.1 × 6.2</td><td>38</td><td>25.02 ± 11.94</td><td>39.59 ± 9.22</td><td>13.6 × 10.0</td><td>39</td><td>71.26 ± 32.10</td><td>105.50 ± 24.77</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>19</td><td>18:14:11.29</td><td>-17:56:00.26</td><td>8.1 × 6.7</td><td>46</td><td>8.36 ± 0.86</td><td>17.54 ± 0.94</td><td>13.9 × 13.1</td><td>20</td><td>0.99 ± 0.30</td><td>2.26 ± 0.30</td><td>**</td><td>CH<sub>3</sub>OH maser</td></tr><tr><td>20</td><td>18:14:14.05</td><td>-17:55:15.15</td><td>26.0 × 20.0</td><td>49</td><td>10.24 ± 3.71</td><td>139.70 ± 8.10</td><td>17.3 × 12.9</td><td>17</td><td>30.22 ± 14.69</td><td>77.31 ± 15.81</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>21</td><td>18:14:13.95</td><td>-17:55:58.44</td><td>12.3 × 10.9</td><td>127</td><td>13.27 ± 2.48</td><td>71.46 ± 4.04</td><td>17.3 × 14.1</td><td>124</td><td>25.97 ± 8.43</td><td>81.02 ± 8.76</td><td>**</td><td>Free-free</td></tr><tr><td>22</td><td>18:14:16.57</td><td>-17:55:29.00</td><td>8.8 × 6.2</td><td>83</td><td>9.77 ± 0.85</td><td>20.98 ± 0.99</td><td>16.0 × 14.3</td><td>138</td><td>1.66 ± 0.33</td><td>4.29 ± 0.33</td><td>**</td><td>Outflows</td></tr><tr><td>23</td><td>18:14:11.14</td><td>-17:55:43.07</td><td>8.6 × 6.5</td><td>62</td><td>20.09 ± 4.38</td><td>38.03 ± 4.25</td><td>11.1 × 9.3</td><td>0</td><td>3.42 ± 0.57</td><td>5.30 ± 0.57</td><td>**</td><td>CO-contaminated</td></tr><tr><td>24</td><td>18:14:10.09</td><td>-17:55:57.82</td><td>10.6 × 6.6</td><td>57</td><td>17.04 ± 2.18</td><td>40.28 ± 2.20</td><td>12.3 × 8.8</td><td>55</td><td>3.32 ± 0.52</td><td>4.51 ± 0.41</td><td>**</td><td>Class I</td></tr><tr><td>25</td><td>18:14:16.25</td><td>-17:55:13.82</td><td>9.7 × 1.3</td><td>153</td><td>21.06 ± 1.08</td><td>21.0 ± 1.08</td><td>13.8 × 11.2</td><td>0</td><td>0.50 ± 0.34</td><td>0.59 ± 0.35</td><td>**</td><td></td></tr><tr><td>26</td><td>18:14:13.46</td><td>-17:55:42.02</td><td>10.2 × 7.7</td><td>56</td><td>60.35 ± 12.55</td><td>113.00 ± 17.71</td><td>13.7 × 12.1</td><td>68</td><td>59.68 ± 43.04</td><td>116.40 ± 33.17</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>27</td><td>18:14:14.10</td><td>-17:55:39.64</td><td>9.1 × 6.5</td><td>83</td><td>52.79 ± 18.23</td><td>113.00 ± 17.71</td><td>–</td><td>–</td><td>≤ 31.000</td><td>≤ 23.880</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>28</td><td>18:14:13.78</td><td>-17:55:41.33</td><td>7.9 × 4.9</td><td>57</td><td>41.09 ± 17.04</td><td>53.23 ± 13.31</td><td>–</td><td>–</td><td>≤ 27.000</td><td>≤ 27.040</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>29</td><td>18:14:12.41</td><td>-17:55:08.30</td><td>10.1 × 7.9</td><td>96</td><td>7.63 ± 1.23</td><td>22.17 ± 1.79</td><td>–</td><td>–</td><td>≤ 0.361</td><td>≤ 0.435</td><td>**</td><td>CO-contaminated</td></tr><tr><td>30</td><td>18:14:11.34</td><td>-17:55:19.55</td><td>10.1 × 9.0</td><td>89</td><td>6.18 ± 0.61</td><td>19.81 ± 0.71</td><td>16.7 × 14.3</td><td>77</td><td>0.70 ± 0.20</td><td>1.98 ± 0.20</td><td>**</td><td></td></tr><tr><td>31</td><td>18:14:17.15</td><td>-17:55:29.83</td><td>6.4 × 4.2</td><td>70</td><td>10.34 ± 0.85</td><td>10.64 ± 0.69</td><td>11.1 × 9.1</td><td>38</td><td>0.81 ± 0.38</td><td>0.97 ± 0.38</td><td>**</td><td></td></tr><tr><td>32</td><td>18:14:15.96</td><td>-17:55:22.22</td><td>9.3 × 6.6</td><td>59</td><td>10.71 ± 1.31</td><td>22.53 ± 1.28</td><td>13.1 × 11.4</td><td>111</td><td>2.09 ± 0.50</td><td>4.41 ± 0.50</td><td>**</td><td></td></tr><tr><td>33</td><td>18:14:13.48</td><td>-17:56:05.49</td><td>9.4 × 8.6</td><td>10</td><td>7.90 ± 1.26</td><td>22.44 ± 1.58</td><td>–</td><td>–</td><td>≤ 0.535</td><td>≤ 0.558</td><td>**</td><td></td></tr><tr><td>34</td><td>18:14:16.55</td><td>-17:56:20.48</td><td>10.2 × 5.7</td><td>66</td><td>5.08 ± 0.40</td><td>11.26 ± 0.46</td><td>–</td><td>–</td><td>≤ 0.024</td><td>≤ 0.025</td><td>**</td><td></td></tr><tr><td>35</td><td>18:14:14.92</td><td>-17:55:48.80</td><td>23.7 × 15.2</td><td>122</td><td>11.15 ± 3.32</td><td>112.20 ± 7.20</td><td>21.7 × 13.3</td><td>117</td><td>26.18 ± 14.58</td><td>97.64 ± 20.25</td><td>**</td><td>Free-free, outflows</td></tr><tr><td>36</td><td>18:14:13.67</td><td>-17:55:23.94</td><td>7.1 × 5.4</td><td>39</td><td>20.96 ± 4.92</td><td>28.47 ± 3.84</td><td>–</td><td>–</td><td>≤ 1.842</td><td>≤ 1.843</td><td>**</td><td></td></tr><tr><td>37</td><td>18:14:15.88</td><td>-17:55:32.39</td><td>8.9 × 6.8</td><td>56</td><td>5.97 ± 0.73</td><td>12.58 ± 0.79</td><td>–</td><td>–</td><td>≤ 0.409</td><td>≤ 0.410</td><td>**</td><td></td></tr><tr><td>38</td><td>18:14:12.28</td><td>-17:55:30.87</td><td>12.6 × 7.0</td><td>39</td><td>3.33 ± 0.99</td><td>3.33 ± 0.99</td><td>–</td><td>–</td><td>≤ 0.191</td><td>≤ 0.192</td><td>**</td><td></td></tr><tr><td>39</td><td>18:14:13.83</td><td>-17:55:52.23</td><td>8.8 × 7.7</td><td>41</td><td>53.00 ± 5.95</td><td>16.6 × 12.6</td><td>–</td><td>–</td><td>20.90 ± 8.34</td><td>54.15 ± 8.36</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>40</td><td>18:14:13.66</td><td>-17:55:26.01</td><td>9.0 × 6.8</td><td>59</td><td>24.71 ± 6.58</td><td>30.67 ± 2.96</td><td>–</td><td>–</td><td>≤ 2.736</td><td>≤ 2.740</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>41</td><td>18:14:11.00</td><td>-17:55:42.02</td><td>6.8 × 5.7</td><td>80</td><td>16.11 ± 3.40</td><td>22.65 ± 3.49</td><td>14.9 × 12.4</td><td>8</td><td>3.30 ± 0.50</td><td>8.08 ± 0.51</td><td>**</td><td>Outflows</td></tr><tr><td>42</td><td>18:14:14.83</td><td>-17:55:32.25</td><td>12.9 × 8.1</td><td>89</td><td>16.64 ± 4.31</td><td>13.65 ± 2.70</td><td>–</td><td>–</td><td>≤ 0.806</td><td>≤ 0.972</td><td>**</td><td>Free-free</td></tr><tr><td>43</td><td>18:14:11.16</td><td>-17:55:39.70</td><td>9.0 × 7.4</td><td>40</td><td>5.06 ± 1.43</td><td>31.21 ± 3.85</td><td>14.1 × 12.1</td><td>21</td><td>3.26 ± 0.56</td><td>7.47 ± 0.56</td><td>**</td><td>Outflows</td></tr><tr><td>44</td><td>18:14:14.24</td><td>-17:55:15.40</td><td>9.8 × 7.6</td><td>59</td><td>14.11 ± 4.09</td><td>15.41 ± 4.42</td><td>11.7 × 8.7</td><td>54</td><td>26.10 ± 6.50</td><td>36.32 ± 6.53</td><td>**</td><td>Free-free</td></tr><tr><td>45</td><td>18:14:14.76</td><td>-17:55:45.88</td><td>12.0 × 8.5</td><td>117</td><td>7.15 ± 4.55</td><td>66.27 ± 5.59</td><td>17.5 × 13.5</td><td>116</td><td>39.16 ± 17.92</td><td>112.10 ± 17.95</td><td>**</td><td>Free-free</td></tr><tr><td>46</td><td>18:14:13.96</td><td>-17:55:31.07</td><td>10.4 × 6.9</td><td>27</td><td>20.82 ± 4.60</td><td>53.37 ± 4.99</td><td>–</td><td>–</td><td>≤ 2.524</td><td>≤ 2.530</td><td>**</td><td>Free-free, outflow ?</td></tr><tr><td>47</td><td>18:14:13.77</td><td>-17:55:31.17</td><td>7.7 × 5.9</td><td>79</td><td>8.40 ± 3.35</td><td>12.45 ± 2.92</td><td>11.4 × 10.4</td><td>95</td><td>22.61 ± 5.02</td><td>34.81 ± 3.87</td><td>**</td><td>Free-free</td></tr><tr><td>48</td><td>18:14:14.39</td><td>-17:55:29.23</td><td>11.3 × 7.9</td><td>43</td><td>5.80 ± 1.74</td><td>15.06 ± 2.04</td><td>–</td><td>–</td><td>≤ 1.431</td><td>≤ 1.435</td><td>**</td><td>Free-free, outflow ?</td></tr></tbody></table>