we solved as an SB1 using a mid-F type HRS template, and three observations with APOGEE that we solved as an SB2 using the BT-Settl templates. These measurements constrained the spectroscopic orbital parameters and allowed us to re-examine our HRS cross-correlation functions and detect the faint companion in two epochs using a mid-M star HRS template and with correlation power slightly above the noise. Table \[rv2445134\] lists the date and corresponding barycentric Julian Date for each of our observations, the RVs we measure, and the associated spectrograph. Figure \[fig:fluxratio\] shows the BT-Settl models corresponding to the primary and secondary components, along with the flux ratio for a synthetic EB constructed from these models. We carried out the MCMC analyses described in §\[mcmcanalysis\] on the RVs in Table \[rv2445134\] and the [*Kepler*]{} photometry, and derived the orbital and physical parameters listed in Table \[orbpar2445134\]. Figures \[fig:model2445lc\] and\[fig:model2445rv\] depict the light and radial velocity curve models, respectively. Due to the large mass ratio, temperature ratio and the orientation of the orbit, the light curve of KIC2445134 contains Doppler boosting. We incorporated Doppler boosting into our model using the framework of @Bloemen2011 and present the Doppler boosting parameters for the primary and secondary 