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tokens: or less blended and we saw only one to three components. Next, we used the least-squares deconvolution (LSD; Donati et al. 1997 ) technique and calculated LSD profiles with the LSD code by Tkachenko et al. ( 2013 ), based on the same line mask as we used for our previously mentioned synthetic spectrum. Figure 1 shows the LSD profiles vertically arranged according to the JD of observation. The resolution is distinctly better than that of the CCFs; four components are now seen in the majority of the LSD profiles. The measured RVs are marked, and the calculated orbital curves plotted in Figure 1 show that we could assign all components in all LSD profiles to four different stars located in two different binary systems, S 1,2 and S 3,4 . Figure 1. LSD profiles calculated from the 29 spectra, vertically arranged according to the JD (2,457,000+) of observation. Measured RVs are marked by open circles and crosses, in the left panel for components C 1 and C 2 and in the right panel for C 3 and C 4 , respectively. The red and green curves illustrate the corresponding, calculated orbital solutions. The RVs of the four components, C 1 to C 4 , were determined by fitting the LSD profiles with multiple Gaussians. The mean (internal) errors of the fit were 0.25, 0.36, 0.28, and 0.37 km s −1 for the RVs of C 1 to C 4 , respectively. We used the method of differential corrections (Schlesinger 1910 ) to determine the orbits from the RVs. Because of the short time span of the observations, this could be done for the two systems separately, without accounting for any interaction between them or for light-travel-time effects. In the case of S 1,2 , we fixed the orbital period to the value known from the Kepler light-curve analysis. The RVs of the four components of KIC 7177553 determined from the multi-Gaussian fit to the LSD profiles are listed in Table 5 in Appendix B . Figure 2 shows the RVs and orbital curves folded with the orbital periods. Table 1 lists the derived orbital parameters. The times of observation of all spectra are based on UTC. To be consistent with the Kepler DCT time scale and the results listed in Table 3 , we added 68 s to the calculated times of periastron passage T . Figure 2. RVs and calculated orbital curves folded with the orbital periods. Left: C 1 (open circles) and C 2 (open squares). Right: C 3 (open circles) and C 4 (open squares). Phase zero corresponds to the time of periastron passage. Table 1 Orbital Solutions Obtained from Multi-Gaussian Fits of the LSD Profiles and with KOREL Note. The table lists period P and orbital elements (eccentricity e , argument of periastron ω , time of periastron passage T , and mass ratio q ) of the two systems, and the RV semiamplitudes K and individual systemic velocities γ . Errors are given in units of the last two digits in parentheses. The last two rows list the rms of the residuals after subtracting the orbital solution from the RVs and the projected masses calculated from the spectroscopic