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Table 3

Conditions in diffuse cloud models and coefficients for departure from LTE of the population in OH levels.

Model 1 Model 2

diffuse molecular translucent
χ [Habing] 1.7 1.7
A V 0.2 1
nH [cm-3] 100 1000
0.1 0.5
Tgas [K] 100 15
Tdust[K] 16 12

departure coefficients

F = 1 − 1.7580 0.9966
F = 2 − 1.7565 0.9963
F = 1 + 1.7398 0.9991
F = 2 + 1.7384 0.9987

Notes. The FUV field is parametrized in units of the Habing field (Draine field = 1.7 Habing, Draine 1978). Defining quantities are from Snow & McCall (2006) and from Voshchinnikov et al. (1999) for the dust temperature. The clouds are immersed in the interstellar radiation field as given by Mathis et al. (1983) and the cosmic microwave background. Departure coefficients are defined as the fractional level population with respect to the population for thermalization at the CMB temperature, 2.73 K.

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