Modeling the molecular gas content and CO-to-H2 conversion factors in low-metallicity star-forming dwarf galaxies

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Volume 681 (January 2024)

A&A, 681 (2024) A14

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Table 2

IR tracers used as constraints and corresponding ionization potentials for ionic lines.

	Tracers
Molecules	CO(1–0)λ2.6 mm
Neutral and ionized gas tracers	[O I]λλ63,145 µm
	[Fe II]λλ17,26 µm (7.9 eV),
	[Si II]λ35 µm(8.2eV),
	[C II]λ158 µm(11.3eV),
	Huαλ12 µm(13.6 eV),
	[N II]λλ122, 205 µm (14.5 eV),
	[Ar II]λ7 µm(15.7eV),
	[Fe III]λ23 µm(16.2eV),
	[Ne II]λ13 µm(21.6eV),
	[S III]λλ19, 33 µm(23.3eV),
	[Ar III]λ 9, 22µm (27.6 eV),
	[N III]λ 57µm (29.6 eV),
	[S IV]λ11 µm(34.7 eV),
	[O III]λ88 µm (35.1 eV),
	[Ne III]λ16 µm (40.9 eV)
	[O IV]λ26 µm (54.9 eV),
	[Ne V]λλ14, 24 µm (97.1 eV),
Total IR luminosity	L_TIR (1–1000 µm)

Notes. We report the ionization potentials corresponding to the energy thresholds required to create the ion producing a given emission line, either by deexcitation or by recombination.

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