Cumulative histograms of minimum mass (left) and semi-major axis (right) of synthetic and observable planets orbiting high-mass stars. In each case, we only take into account planets whose induced Doppler semi-amplitude is larger than 30 m/s, and whose periods are shorter than 3 years. Moreover, we exclude planets located at distances closer than 0.1 AU (the internal limit of our computational disk). For synthetic planets (heavy lines), we used the formation model around 2.0 M⊙ stars, whereas we selected planets discovered around stars with masses of between 1.8 M⊙ and 3.0 M⊙ (step-like lines). The three heavy lines are for the formation model around a 2.0 M⊙ star, for αD equal to 1.2 (solid line), 0 (dotted line), and 2 (dashed line). The thin solid line is for a primary mass of 1.0 M⊙. The results of statistical comparison between the different curves is indicated in Table 2.
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