<table><caption>**Table C.5.** Main characteristics of the 616 prestellar cores in the ALMA-IMF protoclusters.</caption><thead><tr><th>Protocluster name<br>(1)</th><th>Core ID number<br>(2)</th><th>R<sub>out</sub><br>[au]<br>(3)</th><th>T<sup>PPMAP</sup><sub>dust</sub>[1.25"]<br>[K]<br>(4)</th><th>T<sub>dust</sub>(prestellar core)[R<sub>out</sub>]<br>[K]<br>(5)</th><th>M<sub>core</sub>[T<sub>dust</sub>]<br>[M<sub>☉</sub>]<br>(6)</th></tr></thead><tbody><tr><td rowspan="6">G008.67</td><td>3</td><td>2780</td><td>30±3</td><td>28±2</td><td>10.8±1.2</td></tr><tr><td>5</td><td>3900</td><td>27±10</td><td>27±9</td><td>6.3±0.2</td></tr><tr><td>6</td><td>2650</td><td>29±3</td><td>27±2</td><td>5.2±0.9</td></tr><tr><td>8</td><td>2680</td><td>30±11</td><td>27±9</td><td>4.9±0.3</td></tr><tr><td>10</td><td>4120</td><td>30±9</td><td>30±9</td><td>4.5±0.4</td></tr><tr><td>6</td><td>1800</td><td>33±5</td><td>26±3</td><td>10.5±0.6</td></tr><tr><td>G010.62</td><td>8</td><td>2340</td><td>41±6</td><td>39±5</td><td>26.4±0.6</td></tr><tr><td>G327.29</td><td>7</td><td>2400</td><td>29±13</td><td>25±11</td><td>6.7±0.3</td></tr><tr><td rowspan="6">G333.60</td><td>69</td><td>1640</td><td>39±12</td><td>31±9</td><td>5.7±1.2</td></tr><tr><td>20</td><td>2170</td><td>36±13</td><td>31±10</td><td>5.4±0.5</td></tr><tr><td>30</td><td>5240</td><td>37±12</td><td>37±11</td><td>5.3±0.3</td></tr><tr><td>53</td><td>4380</td><td>35±12</td><td>34±11</td><td>4.3±0.5</td></tr><tr><td>34</td><td>2620</td><td>36±12</td><td>31±10</td><td>4.0±0.5</td></tr><tr><td>7</td><td>1890</td><td>35±4</td><td>29±3</td><td>7.0±0.7</td></tr><tr><td rowspan="2">G337.92</td><td>8</td><td>1680</td><td>36±4</td><td>29±3</td><td>6.9±1.0</td></tr><tr><td>12</td><td>2670</td><td>33±4</td><td>30±3</td><td>5.1±0.9</td></tr><tr><td rowspan="2">G338.93</td><td>5</td><td>1600</td><td>35±8</td><td>28±6</td><td>14.1±0.3</td></tr><tr><td>17</td><td>3750</td><td>32±8</td><td>30±7</td><td>4.3±0.2</td></tr><tr><td>G353.41</td><td>6</td><td>2230</td><td>26±6</td><td>25±5</td><td>8.6±0.3</td></tr><tr><td rowspan="8">W43-MM1</td><td>6</td><td>1930</td><td>24±3</td><td>18±2</td><td>45.2±1.1</td></tr><tr><td>134</td><td>2480</td><td>27±3</td><td>22±2</td><td>21.1±2.0</td></tr><tr><td>17</td><td>1820</td><td>27±3</td><td>20±2</td><td>18.2±1.7</td></tr><tr><td>136</td><td>1850</td><td>28±3</td><td>21±2</td><td>12.2±1.9</td></tr><tr><td>21</td><td>1380</td><td>24±4</td><td>17±2</td><td>12.2±0.5</td></tr><tr><td>20</td><td>1410</td><td>24±4</td><td>17±3</td><td>10.3±0.3</td></tr><tr><td>37</td><td>3570</td><td>23±4</td><td>21±3</td><td>6.6±0.3</td></tr><tr><td>22</td><td>3120</td><td>28±4</td><td>24±3</td><td>14.2±0.8</td></tr><tr><td>13</td><td>1280</td><td>24±4</td><td>17±3</td><td>9.3±0.3</td></tr><tr><td rowspan="2">W43-MM3</td><td>11</td><td>2050</td><td>26±7</td><td>20±5</td><td>7.9±0.2</td></tr><tr><td>43</td><td>5350</td><td>26±6</td><td>24±6</td><td>5.5±0.2</td></tr><tr><td rowspan="7">W51-E</td><td>19</td><td>3470</td><td>45±8</td><td>40±6</td><td>65.5±5.2</td></tr><tr><td>37</td><td>2870</td><td>45±8</td><td>38±6</td><td>43.6±4.8</td></tr><tr><td>23</td><td>3300</td><td>44±8</td><td>38±6</td><td>33.3±3.3</td></tr><tr><td>26</td><td>3890</td><td>25±8</td><td>22±7</td><td>13.2±0.9</td></tr><tr><td>29</td><td>1890</td><td>38±8</td><td>30±6</td><td>11.5±2.0</td></tr><tr><td>43</td><td>2820</td><td>34±8</td><td>28±6</td><td>5.3±0.8</td></tr><tr><td>12</td><td>2710</td><td>35±7</td><td>29±6</td><td>16.0±0.7</td></tr><tr><td rowspan="8">W51-IRS2</td><td>10</td><td>2360</td><td>31±8</td><td>25±6</td><td>13.8±0.4</td></tr><tr><td>13</td><td>3640</td><td>33±7</td><td>29±6</td><td>12.7±0.4</td></tr><tr><td>24</td><td>2930</td><td>33±7</td><td>28±5</td><td>9.3±0.5</td></tr><tr><td>39</td><td>2730</td><td>36±6</td><td>30±5</td><td>7.8±0.6</td></tr><tr><td>31</td><td>3140</td><td>28±9</td><td>24±7</td><td>7.3±0.4</td></tr><tr><td>19</td><td>4000</td><td>29±9</td><td>26±7</td><td>6.3±0.2</td></tr><tr><td>80</td><td>3720</td><td>30±8</td><td>27±7</td><td>5.5±0.4</td></tr><tr><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>

**Notes.** (3) Outer radius of cores, assumed to be equal to their FWHM (see Sect. 2.1), deconvolved by the beam and set at their distance to the Sun (Motte et al. 2022). (4) Temperature measured in the PPMAP dust temperature image at core location. (5) Mass-averaged dust temperature of prestellar cores estimated from Eq. (9) using Cols. 3–4. (6) Core mass computed from the fluxes measured in the catalogs listed in Sect. 2.1 and the temperature of Col. 5 in Eq. (11).
**Appendix D: Complementary figures**

Appendix D complements Fig. 1 by presenting in Fig. D.1 all the other coincidences of luminosity peaks with the ALMA-IMF protostellar cores (Nony et al. 2020, 2023, in prep.; Armante et al. 2024; Valeille-Manet et al. 2024). In addition, Fig. D.2 displays the luminosity profiles at four locations encompassing the six brightest hot cores of ALMA-IMF (Bonfand et al. 2024). These profiles are used to estimate the total luminosity of their eight associated protostellar cores, which are listed in Table C.3. And Fig. D.3, published on Zenodo, compares the mass-averaged dust temperature of prestellar cores, whether they are located in luminosity peaks or not.

<figure><img src="image_12.png" /><figcaption>**Fig. D.1.** Zoom into the luminosity and temperature peaks, characterized at 2.5", to identify their associated protostellar and prestellar cores, detected at 0.3" – 0.9" resolution. *Fourteen first panels:* Location of the different zooms on the 1.3 mm image of each ALMA-IMF protocluster. Red squares outline the zooms of Fig. 1 and blue squares the complementary zooms shown here.</figcaption></figure>
<figure><img src="image_13.png" /></figure>

**Fig. D.1. continued.** Zoom-in of regions in ALMA-IMF protoclusters: G008.67 (two panels), G10.62 (two panels), G012.80 (five panels completing Fig. 1a), and G327.29 (three panels). Red and blue contours display the PPMAP luminosity and dust temperature map values, respectively, overlaid on the 1.3 mm continuum map shown in the grayscale background. Orange ellipses outline the FWHM size of the luminosity peaks associated with at least one protostellar core (see Dell'Ova et al. 2024, Tables C.2 and C.7 published at the CDS). White ellipses and crosses locate the protostellar and prestellar cores, respectively, identified by (Nony et al. 2020, 2023, in prep.), Pouteau et al. (2022), Armante et al. (2024), and Louvet et al. (2024). A scale bar is shown in the right-hand side of each panel. Some luminosity (and temperature) peaks host two and up to four protostellar cores of 1900 au typical size (see, e.g., P1 and P4 in G10.62).
<figure><img src="image_14.png" /><figcaption>**Fig. D.1. continued.** Zoom-in of regions in ALMA-IMF protoclusters: G328.25 (one panel), G333.60 (three panels), G337.92.80 (two panels), G338.93 (three panels), G353.41 (two panels), and W43-MM1 (one panel completing Fig. 1b). Some luminosity (and temperature) peaks host two and up to four protostellar cores of 1900 au typical size (see, e.g., P4 in G333.60, P2 in G337.92, and P3 and P10 in G338.93).</figcaption></figure>
<figure><img src="image_15.png" /></figure>

**Fig. D.1. continued.** Zoom-in of regions in ALMA-IMF protoclusters: W43-MM2 (three panels completing Fig. 1c), W43-MM3 (two panels completing Fig. 1d), W51-E (two panels), and W51-IRS2 (five panels). Some luminosity (and temperature) peaks host two and up to four protostellar cores of 1900 au typical size (see, e.g., P1 and P2 in W51-E, P1 and P2 in W51-IRS2).
<figure><img src="image_16.png" /><figcaption>**Fig. D.2.** Luminosity profiles of the four positions at 2.5" resolution encompassing the six brightest ALMA-IMF hot cores (Bonfand et al. 2024). The luminosity is azimuthally averaged at four locations encompassing these hot cores using the median in rings spaced by 1.25" in radius from these locations. Profiles are fitted by the combination of a power-law and a Gaussian.</figcaption></figure>