Table 6
Samples and methods comparison.
| Sample | Host mass | Tech. | Frequency | Sep. range | Planet mass limit | Reference |
| (M⊙) | (AU) | (MJup) | ||||
|
|
||||||
| F5–A0 | ~1.5–3.0 | AO | 5.9–18.8% | 5–320 | 3–14a | this work |
| Evolved A | 1.3–1.9 | RV | 11 ± 2% | 0.1–3 | >0.2–1.3b | Johnson et al. (2010a) |
|
|
||||||
| K7–F2 | 0.7–1.5 | AO | <20% | 25–856 | >4 | Nielsen & Close (2010) |
| FGK | 0.7–1.3 | RV | 6.5 ± 0.7% | 0.01–3 | >0.5–0.9c | Johnson et al. (2010a) |
|
|
||||||
| M5–M0 | 0.2–0.6 | AO | <20% | 9–207 | >4 | Nielsen & Close (2010) |
| M | 0.1–0.7 | RV | 2.5 ± 0.9% | 0.01–3 | >0.1–0.5c | Johnson et al. (2010a) |
Notes.
The detection limit is a function of separation, as detailed in Fig. 7. The frequency estimation is based on a flat distribution for the planets mass.
The detection limit is a function of separation, as reported in Bowler et al. (2010a).
Scaled from the limits in Bowler et al. (2010a) using the fixed RV amplitude cutoff of K > 20 m s-1 reported in Johnson et al. (2010a) and the ratio of the average mass of the bin to the average mass of the evolved A-stars, taken to the power of 2/3.
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