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Fig. 6


Cumulative size distribution of planetesimals. This is the cumulative size distribution of those asteroids that are outsideV shapes and thus probably do not belong to a family. Additionally, in this dataset, are included the parent bodies of families, as originally they belonged to the planetesimal population. The distribution is then corrected for the maximum number of objects that were lost due the collisional and dynamical evolution; this gives an upper limit for the distribution of the planetesimals (open squares). Functions of the form N(> D) = N0Dβ, where N is the cumulative number of asteroids, are fitted piecewise in the size ranges D > 100, 35 < D < 100, and D < 35 km. For the original planetesimals size distribution, we obtain the values of β reported by the labels in the plot. Left panel: correction to the number of asteroids is calculated taking into account 10 Gyr of collisional evolution in the present main-belt environment, following the prescription of Bottke et al. (2005). Right panel: correction to the number of asteroids taking into account 4.5 Gyr of collisional evolution in the present main-belt environment.

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