Modelling the He I triplet absorption at 10 830 Å in the atmospheres of HD 189733 b and GJ 3470 b

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Volume 647 (March 2021)

A&A, 647 (2021) A129

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Table A.1

HST/COS line fluxes of HD 189733.

Ion	λ_model	log T_max	F_obs	S∕N	Ratio	Blends
Ne V	1145.5959	5.5	7.09e-17	4.5	−0.02
Si III	1206.5019	4.9	1.10e-14	39.9	−0.75
O V	1218.3440	5.5	2.19e-15	39.8	0.21
N V	1238.8218	5.4	3.32e-15	25.9	0.05
N V	1242.8042	5.4	1.58e-15	17.6	0.03
S II	1253.8130	4.6	1.56e-16	9.6	0.03
S II	1259.5210	4.6	2.70e-16	11.7	0.04
Si II	1260.4240	4.6	5.00e-16	15.2	−0.78
Si II	1264.7400	4.5	1.95e-15	18.5	0.12	Si II1265.0040
Si III	1296.7280	4.9	1.13e-16	6.6	0.07
Si III	1298.9480	4.9	4.36e-16	7.4	0.37	Si III1298.8940
Si III	1303.3250	4.9	1.36e-16	7.9	0.06
Si II	1309.2770	4.6	6.49e-16	11.0	0.02
C II	1323.9080	4.8	9.90e-17	5.9	−0.40	C II1323.9540
C II	1334.5350	4.7	8.96e-15	33.6	−0.31
C II	1335.7100	4.7	1.72e-14	42.8	0.16	C II1335.6650
Fe III	1364.2950	4.6	1.53e-16	9.8	0.01
O V	1371.2960	5.5	2.96e-16	11.2	−0.02
Si IV	1393.7552	5.0	6.91e-15	25.8	−0.02
O IV	1401.1570	5.3	4.52e-16	10.8	−0.75
Si IV	1402.7704	5.0	3.55e-15	20.1	−0.01
S IV	1406.0160	5.1	6.40e-17	5.8	−0.48

Notes. Line fluxes (in erg cm⁻² s⁻¹) measured in HST/COS HD 189733 spectra. log T_max (K) indicates the maximum temperature of formation of the line (unweighted by the EMD). ‘Ratio’ is the log(F_obs/F_pred) of the line. Blends amounting to more than 5% of the total flux for each line are indicated.

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