Table 1
Results of previous high-resolution searches for reflected light of non-transiting hot Jupiters.
| Planet | Reference | ϵ | Confidence | Phase-function | i (Kp) | Rp (RJ) | p |
|---|---|---|---|---|---|---|---|
| τ Boo b | Charbonneau et al. (1999) | <5 × 10−5 | 99% | Lambertian | ~45° | 1.2 | <0.3 |
| Collier Cameron et al. (2000) | <3.5 × 10−5 | 99.9% | Lambertian | ~40° | 1.2 | <0.22 | |
| Leigh et al. (2003a) | <5.61 × 10−5 | 99.9% | Venus-like | 36° | 1.2 | <0.39 | |
| Rodler et al. (2010) | <5.1 × 10−5 | 99.9% | Venus-like | 46° | 1.2 | <0.40 | |
| 75289 b | Leigh et al. (2003b) | <4.18 × 10−5 | 99.9% | Venus-like | (127 km s−1) | 1.6 | <0.12 |
| Rodler et al. (2008) | <6.7 × 10−5 | 99.9% | Venus-like | (129 km s−1) | 1.2 | <0.46 | |
| υ And b | Collier Cameron et al. (2002) | <5.85 × 10−5 | 99.9% | Venus-like | (135 km s−1) | – | – |
| 51 Peg b | Martins et al. (2015) | 6.0 ± 0.4 × 10−5 | 3.7σ | Lambertian | (132 km s−1) | 1.9 ± 0.3 | 0.5 |
Notes. The last four columns indicate the assumed phase function, the best-fit orbital inclination i (or equivalent: the best-fit semi-amplitude Kp of the radially projected orbital velocity) and the inferred limiting combination of planet radius and grey albedo. The works that use Venus-like phase functions use an empirical model formulated by Hilton (1992). The only work in this list that claims an actual measurement of ϵ is the work by Martins et al. (2015). All other studies report upper limits. The upper limit by Collier Cameron et al. (2000) was adjusted by Leigh et al. (2003a) and is therefore superseded by it. The limit quoted from Charbonneau et al. (1999) is inferred from the inclination-dependent contrast curve presented in their work.
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