and Pravec (2009) that was further developed in Scheirich et al. (2015). In following, we outline the basic points of the method, but we refer the reader to the 2009 and 2015 papers for details of the technique.

The shapes of the binary asteroid components were represented with ellipsoids, orbiting each other on a Keplerian orbit with apsidal precession and allowing for a quadratic drift in mean anomaly. The primary was modeled as an oblate spheroid, with its spin axis assumed to be normal to the mutual orbital plane of the components (i.e., assuming zero inclination of the mutual orbit). The shape of the secondary was modeled as a prolate spheroid in synchronous rotation, with its long axis aligned with the centers of the two bodies (i.e., assuming zero libration). The shapes were approximated with 1016 and 252 triangular facets for the primary and the secondary, respectively. The components were assumed to have the same albedo. The brightness of the system as seen by the observer was computed as a sum of contributions from all visible facets using a ray-tracing code that checks which facets are occulted by or are in shadow from the other body. A combination of Lommel-Seeliger 