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\paragraph{Parameters - SFR, IMF and z}  The authors assume a constant Star Formation Rate (0-12Gyr) and a time independent IMF as per  \cite{kroupa} . 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{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 ad-hoc analyitic analytic  formulae for respectively to  the functionsto  $f(a)$ - initial orbit-sizes, $f(q)$ - initial mass ratios and $f(e)$ - initial eccentricities respectively. eccentricities.  \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).