tokens: the TRES spectra as described by Buchhave et al. ( 2010 ). We derived the RVs by cross correlating each spectrum order by order against the observed spectrum with the highest S/N in the wavelength range of 4520–6280 Å. EPIC 202900527 11 TRES RVs are listed in Table 1 , and the phase-folded RV curve is shown in Figure 2 . The reference (or template) spectrum is at BJD = 2457854.95084 and its RV is listed as 0.0 km s −1 in Table 1 . To allow putting the TRES RVs on an absolute scale, we determined the template spectrum absolute RV by cross correlating it with a synthetic spectrum to be −57.87 ± 0.10 km s −1 . This RV offset is not added to the RVs in Table 1 to avoid inflating their uncertainties. 3. Data Analysis and Results 3.1. Stellar Spectroscopic Parameters We derived the spectroscopic stellar parameters using the SpecMatch package (Petigura 2015 ; Petigura et al. 2017 ) and the iodine-free HIRES spectra of each star. Those include the effective temperature , surface gravity , metallicity [Fe/H], and stellar rotation projected on the line of sight , where V is the equatorial rotation and I is the stellar rotation inclination angle. We averaged the parameters extracted from all of the individual observations. The observation-to-observation parameter variance was smaller than the quoted uncertainties in all cases. The SpecMatch results are listed in Table 2 . Table 2 Fitted and Derived Parameters Notes. a Derived using SpecMatch analysis of the spectra. b Model fit parameters, fitted to the K2 light curve, RVs, and stellar isochrones. Gaussian priors are applied to [Fe/H] using the values derived from the SpecMatch spectroscopic analysis. See Section 3 for more information. c For EPIC 206155547 and EPIC 206432863 γ is the binary system’s center of mass RV since the HIRES RVs are on an absolute scale. For EPIC 202900527 the RV of the template spectrum (−57.87 ± 0.10 km s −1 ; see Section 2.3 ) needs to be added to γ to get the center of mass RV. d Parameter fixed during the model fitting process. e upper limit given when no eclipse was detected. f The transit, or primary eclipse, is at phase zero. 3.2. Global Model Fitting We performed a global modeling of the available photometric and RV measurements, along with the spectroscopic atmospheric properties of the primary star, to derive the parameters for each system. For stellar binaries, the transit-derived orbital semimajor axis normalized by the primary stellar radius is dependent on the sum of the two components’ masses and the volume of the primary star, as per Sozzetti et al. ( 2007 ):where P is the orbital period and G the gravitational constant. To take advantage of this relation, we fit directly for the masses of the two stars, the primary radius, and the secondary-to-primary radii ratio , as well as the standard transit and RV orbital parameters including the orbital period P , mid-transit time T 0 , line-of-sight orbital inclination i , orbital eccentricity parameters and
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