Table 3
Summary of individual line detection in the transmission spectrum of MASCARA-4b.
| Line | λ0 (Å) | h (%) | Nsc | S/N | f | FWHM (km s−1) | vwind (km s−1) |
|---|---|---|---|---|---|---|---|
| Hα | 6564.61 | −0.317 ± 0.021 | 48.4 ± 3.3 | 14.8 | 1.89 | 31.4 ± 2.4 | −3.0 ± 1.0 |
| Hβ | 4862.72 | −0.143 ± 0.030 | 21.9 ± 4.5 | 4.8 | 1.49 | 27.2 ± 8.1 | 4.5 ± 2.3 |
| Ca II H | 3969.59 | −0.705 ± 0.082 | 107.6 ± 12.6 | 8.6 | 1.48 | 23.0 ± 3.0 | 0.2 ± 1.3 |
| Ca II K | 3934.77 | −0.844 ± 0.082 | 128.9 ± 12.5 | 10.3 | 1.31 | 29.6 ± 3.1 | 0.4 ± 1.5 |
| Na I D1 | 5897.55 | −0.168 ± 0.014 | 25.6 ± 2.2 | 11.9 | 1.32 | 28.6 ± 2.8 | −1.8 ± 1.1 |
| Na I D2 | 5891.58 | −0.214 ± 0.017 | 32.7 ± 2.6 | 12.4 | 1.37 | 19.9 ± 2.1 | −3.6 ± 0.7 |
| Mg I | 5174.12 | −0.151 ± 0.017 | 23.0 ± 2.6 | 8.7 | 1.04 | 22.6 ± 3.5 | 1.5 ± 1.3 |
| Mg I | 5185.05 | −0.125 ± 0.019 | 19.1 ± 2.9 | 6.5 | 1.08 | 25.2 ± 5.8 | 2.3 ± 1.6 |
| Fe I | 4046.96 | −0.162 ± 0.025 | 24.8 ± 3.8 | 6.6 | 1.04 | 27.8 ± 4.4 | −5.0 ± 2.1 |
| Fe I | 4384.78 | −0.135 ± 0.016 | 20.6 ± 2.5 | 8.3 | 1.16 | 29.2 ± 4.1 | −0.0 ± 1.6 |
| Fe II | 4925.30 | −0.226 ± 0.022 | 34.5 ± 3.3 | 10.3 | 1.13 | 13.1 ± 1.7 | −0.1 ± 0.6 |
| Fe II | 5019.83 | −0.211 ± 0.020 | 32.2 ± 3.0 | 10.8 | 1.11 | 19.1 ± 2.5 | −0.7 ± 0.8 |
Notes. λ0 is the central wavelength of the line in vacuum. h, FWHM, and vwind are the amplitude, width, and center of the best-fit Gaussian profile to the planetary absorption. S/N is simply calculated as the value of h divided by its uncertainty. Nsc represents the number of atmospheric scale heights that the peak absorption corresponds to. f is the scaling factor applied to the stellar RM+CLV model.
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