Table 1
Observed values of the power-law exponent β (Col. 4) in different phases of the ISM (from diffuse HI gas to GMCs).
| Region | Distance | Tracer | β | Peak 1 | Peak 2 | Reference | |
| [pc] | [pc] | [pc] | |||||
|
|
|||||||
| Diffuse HI | HI | 2.6–2.8 | Green et al. (1993) | ||||
| North Polar Spur | HI | 3.6 | Miville-Deschenes (2003) | ||||
|
|
|||||||
| Diffuse Clouds | |||||||
| Polaris Flare | 150 | 13CO 1 → 0 | 2.77 | Stutzki et al. (1998) | |||
| Polaris Flare | 13CO 2 → 1 | 2.76 | Falgarone et al. (1998), Stutzki et al. (1998) | ||||
|
|
|||||||
| low-mass SF cloud | |||||||
|
|
|||||||
| Perseus | 300 | 13CO 1 → 0 | 3.07 | 2.7 | (>10) | Bensch et al. (2001) | |
| Perseus | 13CO 1 → 0 | 3.09 | Sun et al. (2006) | ||||
| Perseus | 13CO 2 → 1 | 3.03 | Sun et al. (2006) | ||||
| Perseus | 12CO 1 → 0 | 3.08 | Sun et al. (2006) | ||||
| Perseus | 12CO 3 → 2 | 3.15 | Sun et al. (2006) | ||||
| Perseus | extinction | 2.55 | Sun et al. (2006) | ||||
| Perseus | extinction | 2.16 | 2.5 | (>10) | |||
| Taurus | 140 | extinction | 2.20 | 0.5 | 3.5 | ||
| Chameleon | 160 | extinction | 2.25 | 0.4 | 4.6 | ||
| Pipe Nebula | 140 | extinction | 2.36 | 1.5 | 3.8 | ||
| IC 5146 | 400 | extinction | 2.37 | (1.4) | (>4.5) | ||
| Lupus | 100 | extinction | 2.49 | (1.5) | (>10) | ||
| Coalsack | 150 | extinction | 2.57 | – | – | ||
| Corona Australis | 170 | extinction | 2.65 | – | 2.9 | ||
|
|
|||||||
| GMC | |||||||
|
|
|||||||
| W3 | 2200 | extinction | 2.07 | – | 11 | ||
| Cygnus | 1700 | 13CO 1 → 0 | 2.47 | 4 | 40 | this study | |
| Cygnus | extinction | 2.42 | – | – | |||
| Orion A | 450 | 13CO 1 → 0 | 2.54 | – | 6 | Bensch et al. (2001) | |
| Orion A | extinction | 2.49 | – | – | |||
| Orion B | 450 | 13CO 1 → 0 | 2.68 | – | 6 | Bensch et al. (2001) | |
| Orion B | extinction | 2.40 | – | >13 | |||
| Orion A+B | extinction | 2.49 | 17 | ||||
| Mon R2 | 800 | 13CO 1 → 0 | 2.76 | 2.75 | >11 | Bensch et al. (2001) | |
| Mon R2 | extinction | 2.26 | 3.9 | >20 | |||
| Mon OB1 | 800 | extinction | 2.55 | (4) | >10 | ||
| Rosette | 1600 | 13CO 1 → 0 | 2.66 | – | >7.5 | Heyer et al. (2006) | |
| Rosette | extinction | 2.55 | – | – | |||
| NGC 2264 | 800 | 13CO 1 → 0 | 2.54 | – | 6.7 | Bensch et al. (2001) | |
| NGC 2264 | extinction | 2.45 | – | – | |||
| Vela | 700 | extinction | 3.12 | – | >7 | ||
Notes. Values for β obtained from our extinction maps are indicated in bold. Columns 5 and 6 indicate the size scale in parsec where spectra show peak values. Values in parenthesis are less reliable, the spectrum shows no prominent peak there. Values given only for peak 2 indicate that there is only one prominent peak. Note that for Orion we determined β individually for the subregions Orion A and B (for direct comparison with the 13CO data) and for the whole complex, which is also shown in Fig. 4.
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