  We present an analysis of nine bright spectroscopic binaries (HD 1585, HD
6613, HD 12390, HD 39923, HD 55201, HD 147430, HD 195543, HD 202699, HD
221643), which have orbital periods of P > 500 days. These well-separated
binaries are the last stars of our sample that we observed with the TIGRE
telescope obtaining intermediate-resolution spectra of R = 20,000. We applied
the same method as described in our previous publication of this series. For
the analysis of the radial velocity curves, we used the toolkit RadVel, which
allowed us to determine all orbital parameters. Recently published orbital
solutions of some systems from Gaia DR3 agree with our results. However, our
solutions have much smaller uncertainties. We determined the basic stellar
parameters of the primary stars with our automatic script using iSpec. The
parameter determination allowed us to place all nine stars in the
Hertzsprung-Russell diagram. We found that all stars have already evolved to
the giant phase. A comparison with stellar evolution tracks of the Eggleton
code was applied to determine the stellar masses and ages. As a result of our
analysis, we were able to estimate the masses of the secondary stars and the
orbital inclinations of the binary systems.

Solar and Stellar Astrophysics