F}_3 = \ell_3 \left( {\cal F}_{\rm N,1} + {\cal F}_{\rm N,2}\right)$, where ${\cal F}_{\rm N,1}$ is the flux from star 1 emitted towards star 2 and vice versa. This value of ${\cal F}_3$ is then used in the calculation of the observed flux ${\cal F}_{i}$ at time $t_i$ as before, i.e., $${\cal F}_{i} =
\frac{{\cal F}_{i,1} + {\cal F}_{i,2} + {\cal F}_3}{ {\cal F}_{\rm N,1} +
{\cal F}_{\rm N,2}+ {\cal F}_3},$$ where ${\cal F}_{i,1}$ is the flux emitted by star 1 towards the observer at time $t_i$ and similarly for ${\cal
F}_{i,2}$. A complete list of changes in `ellc` version 1.6.1 is provided in the file [CHANGELOG.rst]{} provided with the package distribution.[^4]

The details of the analysis are not the same for every binary system because some binary systems have peculiarities that required special treatment. Here we outline the main features of the analysis applied to the majority of the systems analysed. Additional details and differences from this general approach for individual systems are described in Section \[notes\_sec\].

The free parameters in the model for each binary were: the sum of radii of the stars in units of the semi-major axis – $r_{\rm sum} = (R_1+R_2)/a$, the ratio of the 