Observatorio del Roque de los Muchachos, La Palma and at Sutherland Observatory, South Africa. Both instruments carry an array of eight wide-field cameras, each with a 2048 $\times$ 2048 pixel CCD detector. The majority of the survey has been conducted using 200-mm, f/1.8 lenses combined with a filter that defines a bandpass covering the wavelengths 400-700 nm [@2006PASP..118.1407P]. From July 2012 the WASP-South instrument has used 85-mm, f/1.2 lenses with SDSS r$^{\prime}$ filters [@2014CoSka..43..500S]. A dedicated pipeline is used to perform aperture photometry on the images at the position of catalogued stars within the images. The data are then processed by a detrending algorithm that has been developed from the SysRem algorithm of @2005MNRAS.356.1466T, as described by @2006MNRAS.373..799C.

Light curve modeling \[ellc\]
-----------------------------

We used version 1.6.1 of the `ellc` light curve model to determine the geometry and other parameters for each binary system. Note that the definition of the “third light” parameter used in this version of `ellc` to account for light from other stars in the photometric aperture is different to the one described in . In the new version, third light is described by the parameter $\ell_3$. This parameter is used to calculate the flux $ {\cal
