Table 6.
Characteristics derived by Viaene et al. (2014) and Draine et al. (2014) from infrared data at the position of the CO(2-1) and CO(1-0) detections in 36″ × 36″ and 18″ × 18″ pixels.
| MC13 |
 |
 |
TC | TW | Mdust | Mstar |  |
 |
SFR | Umean | Umin | Tmean | Tmin | SFR |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| ID | 10−2 | 10−3 | K | K | M⊙ | 107 M⊙ | M⊙ Myr−1 | K | K | M⊙ Myr−1 | ||||
| (Viaene et al. 2014) | (Draine et al. 2014) | (F13) | ||||||||||||
| 15 | 4.8 | 4.0 | 29.8 | 63.7 | 33 | 1.8 | 0.152 | 0.022 | 0.22 | 18.6 | 15.0 | 29.3 | 28.3 | 8 |
| 28 | 3.1 | 2.7 | 29.8 | 63.7 | 33 | 1.8 | 0.152 | 0.022 | 0.22 | 32.3 | 22.0 | 32.1 | 30.13 | 77 |
| 36 | 7.8 | 6.6 | 29.8 | 63.7 | 38 | 2.0 | 0.162 | 0.027 | 3.25 | 27.1 | 25. | 31.2 | 30.7 | 133 |
Notes. As described in Sect. 4.1 and in Melchior & Combes (2016), ηbf provides the beam filling factor computed for a brightness temperature of 5 K relying on the RADEX results presented in Sect. 4.1 and 30 K assuming it is thermalised with the dust. The values TC and TW correspond to the cold and warm dust components; Mdust and Mstar are the dust and stellar masses scaled to the prorata of the 12″ CO FWHM beam; and 
and 
are the dust and diffuse dust optical depths, given for the order of magnitude as they are the poorest constrained parameters according to Viaene et al. (2014). The SFR is scaled to the pro rata of the 12″ CO FWHM beam. The last column provides the SFR estimate of Ford et al. (2013) integrated on the 12″ beam.
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