eccentric planets

∼15 MJup, with an upper mass limit corresponding to the (vanishing) tail of
mass distribution. The planet mass distribution is shown in Fig. 1 and follows
wer law, dN/dM ∝ M −1.05 54), 55) affected very little by the unknown sin i. 41)
paucity of companions with Msin i greater than 12 MJup confirms the presence
“brown dwarf desert” 54) for companions with orbital periods up to a decade.
Marcy et al. 2005
Number of Planets
20
15
10
5
Planet Mass Distribution
dN/dM ! M −1.05
104 Planets
Keck, Lick, AAT
0
0 2 4 6 8 10 12 14
M sin i (MJUP) 1. The histogram of 104 planet masses (Msin i) found in the uniform 3 m s −1 Doppler survey
f 1330 stars at Lick, Keck, and the AAT telescopes. The bin size is 0.5 MJup. The distribution
f planet masses rises as M −1.05 from 10 MJup down to Saturn masses, with incompleteness at
ower masses.
Mass distribution: old versions (giants)
•mass distribution from RV observations.
HARPS
•rising towards smaller masses. No obs. bias: smaller masses are more difficult to detect.
•beware of uncorrected (biased) distributions!
•frequency of Jovian planets falls as about M -1 .
•maximum of giant planet masses at about 1 Jupiter mass.
•HARPS gave around 2007 the first hint of a second population of low mass planets.
?
Udry et al. 2007