Table 4
NIR and optical extinction vs. thermal dust emission for four molecular clouds and for the high-latitude diffuse medium.
| Object | Extinction | γ | γ′ | Ref. |
|---|---|---|---|---|
| range (AV) | 104 | |||
| Orion A | ≲5 | 2.20 | 1 | |
| Orion B | ≲6 | 3.09 | 1 | |
| Perseus | ≲6 | 3.51 | 2 | |
| Draco nebula | ≲1.5 | |||
| w. “diffuse dust”* | 4.62 | 0.072 | 3 | |
| w. “molecular dust”** | 3.30 | 0.052 | 4 | |
| LDN 1780 | ≲4 | 0.039 | 5 | |
Notes. The relationship is expressed as AV = γ × τ353GHz + δ and as AV = γ′× I(250 μm) + δ′. (*) Using the γ value as derived for diffuse dust by Planck Collaboration XI (2014) from E(B − V) = 1.49 × 104 τ353GHz and AV ∕E(B − V) = 3.1. (**) Using the mean of the γ values of Orion B and Perseus.
References. (1) Lombardi et al. (2014), (2) Zari et al. (2016), (3) Planck Collaboration XI (2014), (4) Miville-Deschênes et al. (2017), (5) this Paper.
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