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\section{Eclipse Statistics} \section{Population Synthesis}  \paragraph{SFR, \paragraph{Parameters - SFR,  IMF and z} The authors assume a constant Star Formation Rate (0-12Gyr) and a time independent IMF \cite{kroupa_variation_2001} . The metallicity parameter [Fe/H] is constant for the duration of a BSE code run (i.e. it is age-independent and uniform) so the authors combined several runs with different upper and lower IMF limits in order to mimic the observed [Fe/H] distributions.   \paragraph{Binary parameters $f(a, q, e)$} \paragraph{Parameters - orbit-sizes, mass-ratios, eccentricities}  \label{par:_f_a_q_e_}  For the binary runs the authors make simplifying first assumption that the function $f(a,q,e)$ is separable and assign 3 independent ad-hoc analyitic formulae for the  functions to $f(a)$, $f(a)$ [orbit-sizes],  $f(q)$ [initial mass ratios]  and $f(e)$ [initial eccentricities]  respectively. 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).     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).     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.