Supplementary material of ALMA-IMF XVII (Valeille-Manet et al. 2025)

Figures entitled "B1_150_ON_OFF_Noise.png" and "B2_Noise_levels_ALMA-IMF.pdf" correspond to the figures of appendix B of Valeille-Manet et al. 2025. 

Figure B1 presents an example of the method used to estimate the noise in the ALMA-IMF datacubes. Figure B2 presents the derived mean and standard deviation of the noise levels of the CO and SiO/DCN datacubes (i.e. over all velocities of the spectral windows), in the 14 ALMA-IMF regions.

Table entitled "C1_table_proto_candidates.txt" corresponds to the table of appendix C of Valeille-Manet et al. 2025.

Table C1 shows the 100 cores of Louvet et al. 2025 with M > 4 M_{\odot} classified as protostellar core candidates due to an association with an outflow. They are listed with their host region, number, coordinates (ICRS), mass, temperature and size. To compute their masses the same PPMAP temperatures as in Louvet et al. 2025 were used. The error on the masses are computed by taking into account only the uncertainties on the integrated and peak fluxes.

Figures entitled "D1_ionising_vs_Mfin.pdf" and "D2_Proto_time_vs_Mini.pdf" correspond to the figures of appendix D of Valeille-Manet et al. 2025.

Figures D1 and D2 display the fraction of the non-ionising protostellar lifetime as function of the final stellar mass, and the non-ionising protostellar lifetime as function of the initial prestellar mass reservoir.

All figures entitled "EXX_YYY_Source_ZZ.pdf" (E1 to E13) correspond to the figures of appendix E of Valeille-Manet et al. 2025. 

Each figure gives the CO and SiO spectra and the individual molecular outflows maps of every candidate of the survey used to classify them as prestellar. The On and On-Off DCN spectra are also presented with the fit adopted to estimate the Vlsr of each candidate. 

For G008.67 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 39.4, 37.5, 35.0, 38.0 mJy/beam.km/s and SiO sigma = 21.7, 27.7, 21.5, 27.3 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G010.62 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 27.6, 8.6, 20.6, 15.4 mJy/beam.km/s and SiO sigma = 5.6, 7.5, 5.4, 7.2 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G012.80 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 112.3, 64.1, 126.2, 72.8 mJy/beam.km/s and SiO sigma = 26.5, 34.0, 26.2, 33.1 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G327.29 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 48.2, 39.3, 56.1, 37.8 mJy/beam.km/s and SiO sigma = 35.5, 44.7, 35.7, 45.5 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G333.60 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 110.8, 17.0, 98.6, 20.3 mJy/beam.km/s and SiO sigma = 15.8, 20.1, 16.1, 19.8 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G337.92 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 38.8, 16.6, 40.3, 24.4 mJy/beam.km/s and SiO sigma = 9.4, 12.5, 10.2, 12.2 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G338.93 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 69.1, 27.1, 70.0, 27.3 mJy/beam.km/s and SiO sigma = 10.3, 12.7, 11.0, 12.5 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For G353.41 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 95.3, 66.0, 62.9, 64.1 mJy/beam.km/s and SiO sigma = 38.5, 49.8, 38.8, 49.1 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For W43-MM1 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 32.6, 18.6, 49.5, 15.3 mJy/beam.km/s and SiO sigma = 6.4, 7.4, 7.3, 7.2 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For W43-MM2 contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 18.9, 11.0, 18.1, 6.4 mJy/beam.km/s and SiO sigma = 4.4, 5.7, 4.5, 5.7 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For W43-MM3 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 14.3, 12.6, 10.8, 9.0 mJy/beam.km/s and SiO sigma = 5.7, 7.2, 5.5, 7.2 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For W51-E contours are 10, 20, 40, and 80 in units of sigma, with CO sigma = 13.3, 7.5, 25.7, 10.2 mJy/beam.km/s and SiO sigma = 4.7, 6.1, 4.6, 6.0 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

For W51-IRS2 contours are 5, 10, 20, and 40 in units of sigma, with CO sigma = 105.5, 13.8, 44.8, 13.2 mJy/beam.km/s and SiO sigma = 5.9, 7.4, 6.2, 7.5 mJy/beam.km/s for cyan, blue, orange and red contours respectively.

Figures entitled "FXX_YYY_massive_highlight.png" (F1 to F14) corerspond to the figures of appendix F of Valeille-Manet et al. 2025. 

Figures F1 to F14 display the fourteen ALMA-IMF fields with the prestellar cores candidates highlighted in blue with their number. The red and orange cores are all the high-mass and intermediate mass cores above which have been studied and have been associated to an outflow (i.e. protostellar cores). The green cores remaining are all the cores which have not been classified.