Samples and methods comparison.
|Sample||Host mass||Tech.||Frequency||Sep. range||Planet mass limit||Reference|
|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)|
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).
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