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Table 3

Physical properties in subregionsa of W43-MM1.

Approach-1 Approach-2
Cloud Area M cloud b ⟨ nH2 ⟩ c d CFEe M ⋆ f SFEg SFR h M ⋆ f SFEg SFR h
subregion [pc2] [M⊙] [cm-3] [M⊙] [%] [M⊙] [%] [M⊙ Myr-1] [M⊙] [%] [M⊙ Myr-1]
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11)
A 1.06 8570 23.9 ×104 3055 915 10.7 4575 790 9.2 3950
B 1.80 6900 5.0 ×104 645 ±25 2.6 ± 1 38 0.8 ±0.3 190 35 0.7 175
D 6.62 3285 5.8 ×103 <25 <1.5 <15 <0.5 <75 – – –
Ridge 5.75 20350 4.3 ×104 3825 18.8 1195 5.8 5975 1200 5.9 6000
East 3.14 9955 - 190 ±0.5 57 0.6 285 – – –
West 2.74 10650 - 3635 34 1090 10.2 5450 – – –

Notes.

(a)

The cloud subregions are defined in Sects. 4–5 and Fig. 1.

(b)

Mcloud is the mass derived by integrating the column density map built from Herschel images.

(c)

The volumetric density is computed from Cols. 2 and 3 of Table 4 via ⟨ nH2 ⟩ = Mcloud/ Volume.

(d)

Total mass of MDCs in the subregion. Uncertainty is the error on the extraction measurements (plus temperature for N1).

(e)

The core formation efficiency is computed from Cols. 2 and 4 via .

(f)

Stellar mass derived by two approaches explained in Sect. 5.

(g)

The “instantaneous” star formation efficiency is computed from Cols. 2 and 6 (resp. 9) via SFE = M⋆/Mcloud.

(h)

The “instantaneous” star formation rate estimated over a protostellar lifetime of tSF = 0.2 Myr is computed from Col. 6 (resp. 9) via SFR = M⋆/tSF.

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