Table 1
Observability of favorable Hot Jupiters for atmospheric retrieval studies with ground-based high resolution spectroscopy.
| Name | d | Rs | Rp | Ts | Tp | V m star | Km star | ⟨Fp∕Fs⟩ | texp | Visible from ESO? |
|---|---|---|---|---|---|---|---|---|---|---|
| (a.u.) | (R⊙) | (RJ) | (K) | (K) | (mag) | (mag) | (h) | (Yes/No) | ||
| (R = 100 k/50 k) | ||||||||||
| 51 Peg b | 0.052 | 1.27 | 1.90 | 5800 | 1370 | 5.46 | 3.91 | 1e-3 | 6/5 | Yes |
| HD 46375 b | 0.041 | 1.00 | 1.02 | 5200 | 1229 | 7.84 | 6.00 | 4e-4 | 71/61 | Yes |
| HD 73256 b | 0.037 | 1.22 | 1.00 (a) | 5636 | 1545 | 8.06 | 6.26 | 4e-4 | 91/79 | Yes |
| HD 75289 b | 0.046 | 1.25 | 1.03 | 6120 | 1527 | 6.36 | 5.06 | 4e-4 | 29/26 | Yes |
| HD 143105 b | 0.038 | 1.23 | 1.00 (a) | 6380 | 1739 | 6.75 | 5.52 | 5e-4 | 27/23 | No |
| HD 179949 b | 0.045 | 1.19 | 1.05 | 6260 | 1541 | 6.24 | 4.94 | 4e-4 | 26/23 | Yes |
| HD 187123 b | 0.043 | 1.17 | 1.00 (a) | 5714 | 1433 | 7.83 | 6.34 | 4e-4 | 98/85 | No (too low) |
| HD 189733 b | 0.031 | 0.81 | 1.14 | 4880 | 1185 | 7.65 | 5.54 | 7e-4 | 78/68 | Yes |
| HD 209458 b | 0.048 | 1.20 | 1.38 | 6100 | 1467 | 7.63 | 6.31 | 7e-4 | 95/83 | Yes |
| HD 212301 b | 0.036 | 1.25 | 1.07 | 6000 | 1692 | 7.76 | 6e-4 | 37/32 | No (too low) | |
| HD 217107 b | 0.073 | 1.08 | 1.00 (a) | 5666 | 1043 | 6.16 | 4.54 | 2e-4 | 67/58 | No |
| KELT-20 b | 0.054 | 1.56 | 1.74 | 8981 | 2307 | 7.58 | 7.42 | 1e-3 | 43/37 | No (too low) |
| τ Boo b | 0.046 | 1.33 | 1.06 | 6300 | 1624 | 4.49 | 3.36 | 4e-4 | 10/9 | Yes |
| υ And b | 0.059 | 1.63 | 1.00 (a) | 6200 | 1560 | 4.10 | 2.86 | 2e-4 | 14/12 | No (too low) |
| WASP-18 b | 0.021 | 1.23 | 1.17 | 6400 | 2374 | 9.30 | 8.13 | 2e-3 | 22/19 | Yes |
| WASP-33 b | 0.026 | 1.44 | 1.60 | 7400 | 2661 | 8.14 | 7.47 | 2e-3 | 13/11 | No (too low) |
| WASP-76 b | 0.033 | 1.73 | 1.83 | 6250 | 2166 | 9.52 | 8.24 | 2e-3 | 25/21 | Yes |
Notes. For each target the table lists its name, distance to the parent star, radii of the star and the planet, stellar effective temperature, planetary equilibrium temperature, stellar magnitudes in V and K bands, mean planet-to-star flux ratio ⟨Fp∕Fs⟩ calculated between 1 and 5 μm, and exposure time needed to reach an S∕N = 5 for the finally obtained exoplanet spectrum using single CRIRES+ setting. The exposure times are given separately for spectral resolutions R = 100 k and R = 50 k, respectively. The last column contains a flag for the observability of the star at the ESO Paranal observatory (Chile). The two primary targets for CRIRES+ are marked with bold. (a)We assumed Rp = 1.0 RJ due to the lack of information.
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