Table 8
Properties related to radial linewidth and virial parameter profiles of the target clumps.
| Source | M⋆ (a) | Slope(b) | ΔV0.1 pc (b) | Radial variations of αvir∕αcr | |
|---|---|---|---|---|---|
| (M⊙) | (km s−1) | ||||
| G18 (c) | 11 | − | − | >10 in center (<0.1 pc) and ~1–2 at outer envelope (>0.1 pc) | |
| G28 | 23 | −0.01(0.48) | 3.6(0.6) | fluctuate at ~0.5–5 at all radii | |
| G19 | 18 | −0.35(0.40) | 4.2(0.5) | fluctuate at ~0.5–5 at all radii | |
| G08a | 17 | −0.46(0.08) | 4.6(0.3) | >2 in center (<0.2 pc) and ~0.5–2 at outer envelope (>0.2 pc) | |
| G31 | 64 | −0.30(0.14) | 6.3(0.4) | ~1 in center (<0.1 pc) and ~0.5–1 at outer envelope (>0.1 pc) | |
| G08b | 26 | −0.09(0.03) | 3.3(0.1) | ≲1 at all radii | |
| G13 | 19 | −0.56(0.13) | 3.7(0.4) | >2 in center (<0.1 pc) and ~1–2 at outer envelope (>0.2 pc) | |
| G10 | 68 | −0.01(0.13) | 4.7(0.4) | ~0.5 in center (<0.1 pc) and ~1–2 at outer envelope (>0.1 pc) |
Notes. (a) Estimated (single) stellar mass based on interpolating the ZAMS models of Choi et al. (2016), from the clump Lbol listed in Table 6. (b)Fitted slope and linewidth amplitude at 0.1 pc (and errors) of the linewidth radial profile in the inner region. The fitted relation is indicated as the dash-dotted line in the upper panel of Fig. 21. (c) For G18, the parameters cannot be properly constrained in the same manner as the other clumps (see Sect. 4.3) and are omitted.
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