PDRs4All - VIII. Mid-infrared emission line inventory of the Orion Bar

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Volume 687 (July 2024)

A&A, 687 (2024) A86

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Table 2

H₂ excitation temperatures and column densities derived from the two linear components of the excitation diagram fits.

	$T_{1}^{*}$ (K)	$T_{2}^{*}$ (10³ K)	log N₁(H₂) (cm⁻²)	log N₂(H₂) (cm⁻²)	$T_{1}^{}$* (K)	$T_{2}^{}$* (10³ K)	log N₁(H₂) (cm⁻²)	log N₂(H₂) (cm⁻²)
	No attenuation correction				With example attenuation correction^(a)

HII	659 ± 54	2.45 ± 0.13	20.10 ± 0.20	17.42 ± 0.11	661 ± 57	2.44 ± 0.16	20.45 ± 0.20	17.85 ± 0.12
Atomic	722 ± 50	2.70 ± 0.05	19.96 ± 0.18	17.31 ± 0.04	728 ± 54	2.71 ± 0.05	20.24 ± 0.19	17.65 ± 0.04
DF1	706 ± 35	2.68 ± 0.04	20.44 ± 0.15	17. 62 ± 0.04	713 ± 41	2.70 ± 0.07	20.95 ± 0.16	18.22 ± 0.05
DF2	666 ± 36	2.90 ± 0.09	20.80 ± 0.17	17.75 ± 0.07	671 ± 40	2.87 ± 0.04	21.27 ± 0.18	18.31 ± 0.04
DF3	661 ± 40	2.66 ± 0.05	20.77 ± 0.18	17.82 ± 0.05	664 ± 43	2.67 ± 0.06	21.06 ± 0.19	18.16 ± 0.06

Notes. ^(a) Example correction assuming a screen geometry, with an attenuation curve and 10 µm silicate feature equal to the Milky Way extinction average of Gordon et al. (2023) with R(V) = 5.5. This results in large A(V) values, e.g., A(V) ~ 20 for DF3.

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