Table 2
Compilation of values of the mass absorption coefficient κν (in cm2 g−1, expressed per gram of gas and dust) used in dense core studies.
| 250 μm | 350 μm | 500 μm | 1250 μm | Reference |
|---|---|---|---|---|
| 0.10 | 5.1(–2) | 2.5(–2) | 4.0(–3) | (1) |
| 0.125 | 6.4(–2) | 3.1(–2) | 5.0(–3) | (2) |
| 0.14 | 7.1(–2) | 3.5(–2) | 5.6(–3) | (3) |
| 0.09 | 4.7(–2) | 2.3(–2) | 3.7(–3) | (4)† |
| 0.05 | 2.6(–2) | 1.3(–2) | 2.0(–3) | (5)‡ |
| 0.10 | 5.2(–2) | 2.6(–2) | 4.0(–3) | (5)‡ |
| 0.2 ± 0.1 | 1.0(–1) | 5.0(–2) | 8.0(–3) | (6) |
| 0.2 ± 0.1 | 9.2(–2) | 4.1(–2) | 4.9(–3) | (6)§ |
| 0.09 | 5.5(–2) | 3.1(–2) | 7.5(–3) | This work|| |
Notes. The values assume β = 2 (see Eq. 2). Numbers in parentheses are powers of ten. (†) Using their relation τ(250) = 2.16 × 10−25NH cm2∕H and assuming 10% of He atoms with respect to hydrogen nuclei. (‡) Values are from their model calculations (their Table 1); values from the synthesized samples, which are probably more emissive than interstellar dust grains, are higher by factors of 4 to 10. (§) Using β = 2.3 as obtained from their study of the dust emission at 1.2 and 2 mm. (||) Using β = 1.56 as obtained from our continuum fit.
References. (1) Hildebrand (1983), (2) Tafalla et al. (2004), (3) Roy et al. (2014), (4) Juvela et al. (2015b), (5) Demyk et al. (2017), (6) Chacón-Tanarro et al. (2017).
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