PDRs4All - X. ALMA and JWST detection of neutral carbon in the externally irradiated disk d203-506: Undepleted gas-phase carbon

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Volume 689 (September 2024)

A&A, 689 (2024) L4

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Table I.1.

Spectroscopic parameters (from NIST⁵ and Haris & Kramida 2017) of the neutral carbon lines discussed in the text, intensities of the lines detected by JWST and ALMA in d203-506, and model predictions.

λ^a (μm)	Transition (u−l)	E_u/k_B (cm⁻¹)	A_ul (s⁻¹)	$I_{obs, b}^{ON - OFF}$ $I_\mathrm{obs\,,\,\it{b}}^{\mathrm{ON-OFF}}$ (1σ error)	$I_{corr b, c}^{ON - OFF}$ $I^{\mathrm{ON-OFF}}_\mathrm{corr\,\it{b,\,c}}$	I_{PDR model, b, d}	I_{PDR model, b, e}
609.1354	(2p²) ³P₁ – (2p²) ³P₀	16.4	7.93E-08	1.62E-06 (9.77E-8)	1.62E-06	(1.60–1.64)E-06	(1.60–1.64)E-06
370.4151	(2p²) ³P₂ – (2p²) ³P₁	43.4	2.65E-07			(0.95–1.03)E-05	(0.95–1.03)E-05

0.982682	(2p²) ¹D₂ – (2p²) ³P₁	10192.6	7.30E-05
0.985296	(2p²) ¹D₂ – (2p²) ³P₂	10192.6	2.20E-04

0.984 (sum)	(2p²) ¹D₂ – (2p²) ³P₂			4.18E-04 (1.81E-05)	8.51E-04	(2.14–4.90)E-04	(1.07–2.04)E-05

0.872953	(2p²) ¹S₀–(2p²) ¹D₂	21648.0	6.00E-01	†	†	(3.49–6.84)E-05	(0.90–1.07)E-06

1.068601	(3p) ³D₂ – (3s) ³P $_{1}^{o}$ $^{\mathrm{o}}_{1}$	69710.6	1.40E+07
1.068827	(3p) ³D₁ – (3s) ³P $_{0}^{o}$ $^{\mathrm{o}}_{0}$	69744.1	1.04E+07
1.069417	(3p) ³D₃ – (3s) ³P $_{2}^{o}$ $^{\mathrm{o}}_{2}$	69744.1	1.84E+07
1.071027	(3p) ³D₁ – (3s) ³P $_{1}^{o}$ $^{\mathrm{o}}_{1}$	69689.5	7.50E+06
1.073247	(3p) ³D₂ – (3s) ³P $_{2}^{o}$ $^{\mathrm{o}}_{2}$	69710.6	4.40E+06
1.075692	(3p) ³D₁ – (3s) ³P $_{2}^{o}$ $^{\mathrm{o}}_{2}$	69689.5	4.80E+05

1.069 (sum)	(3p) ³D – ³P⁰			1.67E-04 (3.67E-05)	3.23E-04	(1.60–2.92)E-04	(2.36–2.51)E-06

1.175145	(3d) ³F $_{2}^{o}$ $^{\mathrm{o}}_{2}$ – (3p) ³D₁	78199.1	2.29E+07
1.175653	(3d) ³F $_{4}^{o}$ $^{\mathrm{o}}_{4}$ – (3p) ³D₃	78249.9	2.60E+07
1.175800	(3d) ³F $_{3}^{o}$ $^{\mathrm{o}}_{3}$ – (3p) ³D₂	78215.5	2.40E+07
1.178077	(3d) ³F $_{2}^{o}$ $^{\mathrm{o}}_{2}$ – (3p) ³D₂	78199.1	2.90E+06
1.180431	(3d) ³F $_{3}^{o}$ $^{\mathrm{o}}_{3}$ – (3p) ³D₃	78215.5	1.26E+06
1.182727	(3d) ³F $_{2}^{o}$ $^{\mathrm{o}}_{2}$ – (3p) ³D₃	78199.1	2.90E+03

1.176 (sum)	(3d) ³F^o – ³D			1.71E-05 (9.87E-06)	3.08E-05	(3.61–5.96)E-05	(1.05–1.14)E-06

1.350596	(4s) ³P $_{2}^{o}$ $^{\mathrm{o}}_{2}$ – (3p) ³S₁	78148.1	6.60E+06
1.356337	(4s) ³P $_{1}^{o}$ $^{\mathrm{o}}_{1}$ – (3p) ³S₁	78116.7	6.50E+06
1.358506	(4s) ³P $_{0}^{o}$ $^{\mathrm{o}}_{0}$ – (3p) ³S₁	78105.0	6.60E+06

1.355 (sum)	(4s) ³P^o – (3p) ³S			2.82E-05 (5.75E-06)	4.55E-05	(2.55–4.75)E-05	(1.71–1.60)E-07

Notes. ^aWavelengths in a vacuum. †Observed with MUSE (Haworth et al. 2023) and quoted also as the [C I] 8729 Å line. ^bIn units of erg cm⁻² s⁻¹ sr⁻¹. ^cAdopting A_V = 1.5 mag of foreground extinction (see text). ^dLine intensity predicted by the reference PDR model (including C⁰ FUV-pumping and C⁺ recombination cascades) with G₀ ≃ (1–2)×10⁴, n_H = 10⁷ cm⁻³, and x_C = 1.4×10⁻⁴. ^e Same but neglecting FUV-pumping of C⁰ lines.

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