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Table 1.

Atomic data for the UV transitions taken from the NIST database (https://www.nist.gov/pml/atomic-spectra-database/).

Transition Wavelength Aul flu σX, 0 Lower level Upper level λmin λmax adust log ϵX δX, 0
(Å) (s−1) (10−13 cm2) (Å) (Å)
H I Lyα 1215.67 6.265 × 108 0.416 0.38 1s2S 1/2 2p2P0 3/2 1200 1230 0.32 12.0 –
Si IIλ1190 1190.42 6.53 × 108 0.277 0.25 3s23p2P0 1/2 3s3p22P 3/2 1170 1210 0.32 7.51 0.85
Si II( * )λ1194 1194.50 3.45 × 109 – – 3s23p2P0 3/2 3s3p22P 3/2
Si IIλ1193 1193.28 2.69 × 109 0.575 0.51 3s23p2P0 1/2 3s3p22P 1/2
Si II( * )λ1197 1197.39 1.40 × 109 – – 3s23p2P0 3/2 3s3p22P 1/2
Si IIλ1260 1260.42 2.57 × 109 1.22 1.16 3s23p2P0 1/2 3s23d2D 3/2 1245 1275 0.32 7.51 0.85
Si II( * )λ1265 1265.02 4.73 × 108 – – 3s23p2P0 3/2 3s23d2D 3/2
C IIλ1334 1334.53 2.42 × 108 0.129 0.13 2s22p2P0 1/2 2s2p22D 3/2 1320 1350 0.35 8.43 0.30
C II( * )λ1335 1335.67 4.76 × 107 0.127 – 2s22p2P0 3/2 2s2p26D0 3/2
Fe IIλ2587 2586.65 8.94 × 107 0.072 0.14 3d64s6D 9/2 3d64p6D0 7/2 2570 2640 0.50 7.50 0.95
Fe II( * )λ2612 2612.65 1.20 × 108 – – 3d64s6D 7/2 3d64p6D0 7/2
Fe II( * )λ2632 2632.11 6.29 × 107 – – 3d64s6D 5/2 3d64p6D0 7/2
Fe IIλ2600 2600.17 2.35 × 108 0.239 0.47 3d64s6D 9/2 3d64p6D0 9/2
Fe II( * )λ2626 2626.45 3.52 × 107 – – 3d64s6D 7/2 3d64p6D0 9/2
Mg IIλ2796 2796.35 2.60 × 108 0.608 1.27 2p63s2S 1/2 2p63p2P0 3/2 2770 2820 0.54 7.60 0.80
Mg IIλ2804 2803.53 2.57 × 108 0.303 0.64 2p63s2S 1/2 2p63p2P0 1/2

Notes. Columns from left to right: notation of each transition, rest-frame wavelength of the resonant or fluorescent (labelled with an asterisk) transition, Einstein coefficient Aul, oscillator strength flu, cross-section at line centre (assuming a Doppler parameter of b = 20 km s−1; see Section 3.1), transition’s lower level, transition’s upper level, wavelength range used for the RT simulation of each transition (λmin and λmax), dust albedo adust (Li & Draine 2001), and gas-phase logarithmic solar abundances (following Asplund et al. 2009, log ϵX = log(X/H)⊙ + 12 where (X/H)⊙ is the relative solar number densities of species X and hydrogen). The last column lists for all species the number fraction of atoms that are depleted onto dust, δX, 0, based on MW measurements by Roman-Duval et al. (2022).

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