Table 2
Parameters of high-mass parts of observational CMFs in some SF regions.
| SF region | Ref. | Γ | Mch | Tracer | Core sizes | Bound? |
|---|---|---|---|---|---|---|
| # | [M⊙] | [ pc ] | ||||
| Sample | 1 | − 1.45 | 10.0 | C18O | 0.08–0.45 | Most? |
| OMC-1 | 2 | − 1.40 | 4.8 | C18O | ~0.2 | Yes |
| S 140 | 3 | − 1.10 | 30.0 | C18O | 0.2–0.6 | Yes |
| Pipe | 4 | − 1.30 | 2.3 | Dust extinction | 0.1–0.4 | ? |
| Perseus, Serpens and Oph | 5 | − 1.30 | 0.9 | Dust emission | ~0.08 | Most |
| Orion A | 6 | −1.40 | 4.0 | Dust emission | 0.03−0.09 | Yes |
| ρ Oph | 7 | − 1.50 | 0.5 | Dust emission | ≲0.01−0.1 | Most |
| Vela-C | 8 | − 1.10 | 5.0 | Dust emission | 0.03−0.3 | Yes |
Notes. These are used for comparison with modeled CMFs in Fig. 5. All estimates are taken from the corresponding bibliographic source.
References.(1) Tachihara et al. (2002); (2) Ikeda & Kitamura (2009); (3) Ikeda & Kitamura (2011); (4) Alves et al. (2007); (5) Enoch et al. (2008); (6) Polychroni et al. (2013); (7) Motte et al. (1998); (8) Giannini et al. (2012).
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