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For the binary runs the authors make simplifying first assumption that the function $f(a,q,e)$ is separable and assign 3 ad-hoc analyitic formulae for the functions to $f(a)$ - initial orbit-sizes, $f(q)$ - initial mass ratios and $f(e)$ - initial eccentricities respectively.  \paragraph{}  All parameters for the BSE code are kept at the defaults and in order to handle brown dwarfs below $0.08 M_{\odot}$ the authors use an extra data grid due to Baraffe et al. (1998).  \paragraph{}  For orbital periods above 5 years, each binary component is evolved separately and a binary is made from two single-star models (S+S) using approximations given by Hurley et al. (2000).  \paragraph{}  The authors have used this parallel S+S approximation as a check on the full BSE models and find the S+S approach gives a roughly similar a-distribution but slightly more short-period pairs then the more detailed BSE calculations.