Table 2
Characterization of the CMF and η-PDF, and evaluation of the evolutionary stage of the parsec-scale subregions of W43-MM2&MM3.
| Subregion name | Core mass range | α |  offset |
Fitted range (s2) | s2 | Fitted range (s3) | s3 | fproto | Evolutionary stage |
|---|---|---|---|---|---|---|---|---|---|
| (M⊙) | (×1021 cm−2) | (×1021 cm−2) | (×1021 cm−2) | (%) | |||||
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) |
| CMF high-mass ends close to the Salpeter slope or steeper | |||||||||
| Outskirts | 0.45–3.4 |  |
55 ± 10 | 100–550 | >−5 | – | – | 7% ± 1 | Quiescent |
| MM51 | 0.6–4.3 |  |
55 ± 10 | 100–250 | >−5 | 250–900 | −0.8 ± 0.2 | 25% ± 5 | Quiescent |
| MM10 | 0.65–11.2 |  |
70 ± 15 | 100–300 | −2.4 ± 0.2 | 300–3000 | −0.9 ± 0.3 | 21% ± 2 | Pre-burst? |
| Top-heavy CMFs | |||||||||
| MM12 | 0.75–17.8 |  |
70 ± 15 | 100–500 | −2.1 ± 0.3 | 500–2200 | −0.1 ± 0.2 | 41% ± 5 | Main-burst? |
| MM2 | 1.1–69.9 |  |
100 ± 20 | 150–1000 | −0.6 ± 0.2 | 1000–26 000 | −0.2 ± 0.3 | 37% ± 2 | Main burst |
| MM3 | 1.1-44.6 |  |
100 ± 20 | 150–1200 | −0.8 ± 0.2 | 1200–8000 | −0.7 ± 0.3 | 22% ± 3 | Post-burst |
| Total | 0.8–69.9 |  |
70 ± 15 | 100–1000 | −0.9 ± 0.3 | 1000–26 000 | −0.3 ± 0.2 | 27% ± 3 | – |
Notes. (2) Mass range used to fit a power law to the subregion CMF. The lower limit of this mass range is the 90% completeness limit of each subregion, with an error of ±0.2 M⊙ (see Pouteau et al. 2022). Its upper limit corresponds to the maximum mass of cores detected in the subregion. (3) Power-law index of the high-mass end of the subregion CMF in its cumulative form, N(> log M) ∝ Mα, measured over the mass range of Col. 2. Uncertainties are estimated by taking into account the fit uncertainties associated with the small-sample statistics, the completeness limit uncertainty of Col. 2, and by varying core masses according to flux, dust temperature, and emissivity uncertainties (see Sect. 3.1.2). (4) Column density offset assumed to correspond to the background of each subregion and used in Eq. (1) to compute their PDF (see Sect. 2.3). (5) and (7) Ranges of column density used to fit two consecutive power laws to the subregion η-PDF tail. The limits of these ranges are defined in Sect. 3.2. (6) and (8) Power-law indices of second and third tails of the subregion η-PDF, 
(see Sect. 3.2), measured over the column density ranges of Cols. 5 and 7, respectively. Uncertainties are estimated by varying the number of bins, the limits of the fitted ranges, and the column density offset of Col. 4. (9) Protostellar fraction of the core catalog above 0.8 M⊙, as derived from the pre-stellar versus protostellar nature of cores determined by Nony et al. (2023). (10) Subregion evolutionary stage defined in Sect. 4.3, based on the ratio of pre-stellar versus protostellar cores (Col. 9), the surface number density of cores (Col. 8 of Table 1), and the presence of HII regions.
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