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Table 4

Main characteristics (size and mass) of the massive protocluster clouds imaged by ALMA-IMF and their evolutionary stage.

Protocluster Imaged areas(1) Refined
cloud name [pc × pc] within A1.3mm over A1.3 mm evolutionary
A1.3mm A3 mm [Jy] [×103M] over A1.3mm [Jy pc−2] stage (5)
W4-MM1 3.1 × 2.3 5.1 × 4.0 80.3 13.4 13 0.005 IR-quiet = Y
W4-MM2 2.6 × 2.4 5.1 × 4.0 69.6 11.6 15 0.009 IR-quiet = Y
G338.93 1.6 × 1.6 2.9 × 2.8 84.6 7.1 7.2 0.02 IR-quiet = Y
G 28.25 1.4 × 1.4 2.2 × 1.9 73.2 2.5 8.3 0.03 IR-quiet = Y
G337.92 1.2 × 1.1 2.1 × 2.0 63.3 2.5 5.8 0.04, faint H II IR-bright → Y
G327.29 1.3 × 1.3 1.9 × 1.8 147.9 5.1 11 0.1, faint H II IR-bright → Y

G351.77 1.3 × 1.3 1.8 × 1.7 158.7 2.5 8.3 0.2, UCH II IR-bright → I
G008.67 2.2 × 1.4 3.1 × 2.1 66.5 3.1 3.2 0.6, UCH II IR-quiet → I
W43-MM3 2.7 × 2.4 5.1 × 4.0 43.2 5.2 2.2 0.2, UCH II IR-bright → I
W51-E 2.6 × 2.4 4.2 × 3.9 278.9 32.7 2.2 1, two HCH II + H II IR-bright → I
G353.41 1.3 × 1.3 1.8 × 1.7 153.4 2.5 1.9 0.7, UCH II + H II IR-bright → I

G010.62 2.3 × 2.2 3.8 × 3.6 87.3 6.7 1.8 2, two H II IR-bright = E
W51-IRS2 2.6 × 2.4 4.2 × 3.9 224.4 20.6 1.4 2, two H II IR-bright = E
G012.80 1.5 × 1.5 2.2 × 2.1 255.4 4.6 1.1 7, H II IR-bright = E
G333.60 2.9 × 2.9 3.9 × 3.7 216.3 12.0 0.8 5, H II IR-bright = E

Notes. (1)Physical areas encompassing the combined primary beam of the 1.3 and 3 mm mosaics, down to 15%. These areas define the cloud sizes. (2)Integrated flux density at 870 μm measured on the ATLASGAL images (Schuller et al. 2009) within the area of the 1.3 mm ALMA images (Col. (2)). (3)Cloud mass computed from the 870 μm integrated flux (Col. (4)) assuming and using Tdust = 20 K, 25 K and 30 K for the Young, Intermediate, and Evolved regions (see Col. (8)), respectively. (4)Flux surface density of the free-free emission at 92.034 GHz, estimated from the integrated flux of the H41α recombination line. Spatial distribution of the ionized gas: HCH II and UCH II consist of <0.05 pc and ~0.1 pc bubbles of ionized gas, respectively; H II are larger regions of ionized gas with a non-spherical structure, some are faint H II regions (see Sect. 4.1 and Motte et al. 2018a). (5)Classification of the ALMA-IMF protocluster clouds: Young (Y), Intermediate (I), and Evolved (E). Their evolutionary stage is refined from that of Csengeri et al. (2017) by measuring their 1.3 mm to 3 mm flux ratio (Col. (6)) and their estimated free-free emission flux density (Col. (7)). We assume that IR-quiet and IR-bright ATLASGAL clumps are associated with Young and Evolved clouds, respectively. Any evolution of this classification is discussed in Sect. 4.1 and indicated here by an arrow.

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