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Table 7
CMF determinations in nearby star-forming regions.
| Region | Distance | Beam size | CMF (a) | Reference |
|---|---|---|---|---|
| (pc) | ||||
| Pipe Nebula | 160 | ~0.03 pc | Shifted IMF | Alves et al. (2007) |
| Orion regions | ~400 | 14′′ at 850 μm | Shifted IMF | Nutter & Ward-Thompson (2007) |
| Polaris Flare | 150 | 18′′ at 250 μm | Shifted IMF | André et al. (2010) |
| Aquila Rift | 260 | 18′′ at 250 μm | α = −2.33 ± 0.06 | Könyves et al. (2015) |
| Orion A | ~400 | 18′′ | α ~−2.3 | Ikeda et al. (2007) |
| Perseus, Serpens, Ophiuchus | 125–260 | 31′′ | α = −2.3 ± 0.4 | Enoch et al. (2008) |
| Taurus L1495 cloud (b) | 140 | ~18′′ | IMF | Marsh et al. (2016) |
Notes. (a) Shifted IMF means that the whole CMF approximates a standard IMF when shifted to lower masses. (b)Sources retrieved using the getsources algorithm of Men’shchikov et al. 2012.
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