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Fig. 6


Eccentricity distribution of the simulated planets within a distance of 5.2 AU from their host star with masses of at least 0.5 Jupiter masses as well as of RV observations of giant planets with masses between 0.5 and 1.25 Jupiter masses exterior to 0.1 AU. We show in colour the different damping rates and systems with initially 15, 30 and 60 embryos (from top to bottom).

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