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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)



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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