Table 3
Results from the fitted model of synthetic spectra of WASP-189 compared with the input parameters.
| Parameter | Input | Broadened (a) | F*,N (3 transits)(b) | F*,N (S/N = 50) (c) | Non-broadened (S/N=50)(d) |
|---|---|---|---|---|---|
| Teff [K] | 8000 | 8400 ± 30 | 8100 ± 50 | 7990 ± 10 | 8000.0 ± 3.3 |
| log g | 3.9 | 4.05 ± 0.02 | 3.94 ± 0.05 | 3.87 ± 0.01 | 3.900 ± 0.003 |
| υ sin i [km/s] | 97.1 ± 0.2 | 6.51 ± 0.07 | 6.83 ± 0.02 | 0.00 ± 0.07 | |
| [Fe/H] [dex] | 0.29 | 0.67 ± 0.02 | 0.42 ± 0.03 | 0.304 ± 0.006 | 0.288 ± 0.002 |
| [Mg/H] | 0.29 | 0.921 ± 0.008 | 0.44 ± 0.02 | 0.289 ± 0.006 | 0.30 ± 0.01 |
| [Ca/H] | 0.29 | 1.234 ± 0.005 | 0.43 ± 0.02 | 0.304 ± 0.005 | 0.283 ± 0.008 |
| [Ti/H] | 0.29 | 1.79 ± 0.01 | 0.37 ± 0.03 | 0.263 ± 0.009 | 0.298 ± 0.01 |
Notes. Individual chemical abundances are reported relative to solar abundances from Grevesse et al. (2007). The uncertainties are statistical uncertainties reported by PySME and do not take any propagated errors into account. (a)The mean out-of-transit-broadened spectrum from three mock transits. (b)The isolated spectrum, F*,N, from three mock transits. (c)The true isolated spectrum, F*,N, with arbitrary noise with S/N=50 added. (d)The non-broadened spectrum with S/N=50.
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