tokens: red giant clump (RGC), with its known de-reddened color and magnitude, in the CMD serves as a reference for the color and magnitude calibration. In the first step of the method, we estimated the combined (instrumental) flux from the source stars, F S, p = F S 1 , p + F S 2 , p , and the companion/primary flux ratio, q F, p , by fitting the KMTC photometry data set processed using the pyDIA code. Here the subscript “ p ” denotes the passband of observation. The measured values are ( F S, I , F S, V ) = (0.07751 ± 0.00060, 0.00909 ± 0.00032) and ( q F, I , q F, V ) = (0.0471 ± 0.0023, 0.0110 ± 0.0084). We note that the value of q F, I , which is derived from the pyDIA reduction, is slightly different (less than 1 σ ) from the value presented in Table 3 , which is derived from the pySIS reduction, because they come from different reductions of the data. Then, the flux values from S 1 and S 2 were estimated by respectively. From the measured flux values in the I - and V -bands, we estimated the colors and magnitudes of S 1 and S 2 to be ( V − I , I ) S 1 = (2.289 ± 0.043, 20.827 ± 0.010) and ( V − I , I ) S 2 = (3.868 ± 0.831, 24.143 ± 0.053), respectively. In Fig. 9 , we mark the locations of S 1 and S 2 with respect to the RGC centroid in the instrumental CMD that was constructed using the pyDIA photometry of the KMTC data (gray dots). Fig. 9. Locations of the primary and companion source stars with respect to the centroid of the RGC in the instrumental CMD (gray dots). The determinations of the source positions and the construction of the CMD are based on the pyDIA photometry of the KMTC data set. We also present the Hubble Space Telescope CMD ( Holtzman et al. 1998 , brown dots) to show the source locations on the main-sequence branch. Although the V -band flux of S 2 has a relatively large fractional (magnitude) error, it is strongly constrained to be faint in an absolute sense. In particular, we find (i.e., a 4.4 σ difference). This serves as a second line of evidence that the 2L2S solution is correct. If, for example, we had somehow missed a 3L1S solution, and the derived 2L2S solutions were merely mimicking it, then q F, I − q F, V should be consistent with zero because there is only one source with just one color. However, according to Eq. ( 4 ), this possibility is excluded at 4.4 σ . In the second step, we calibrated the color and magnitude. With the measured instrumental color and brightness of the source, ( V − I , I ), and the RGC centroid, ( V − I , I ) RGC = (2.473, 16.918), together with the known de-reddened values of the RGC centroid, ( V − I , I ) RGC, 0 = (1.060, 14.509) ( Bensby et al. 2013 ; Nataf et al. 2013 ), the reddening and extinction corrected color and magnitude of the source were estimated by where Δ( V − I , I ) denote the offsets in the color and brightness of the source from the RGC centroid measured on the instrumental CMD. This results in In Table 5 , we summarize the values of ( V − I , I ) RGC , ( V − I , I
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