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We present an analysis of nine bright spectroscopic binaries (HD 1585, HD6613, HD 12390, HD 39923, HD 55201, HD 147430, HD 195543, HD 202699, HD221643), which have orbital periods of P > 500 days. These well-separatedbinaries are the last stars of our sample that we observed with the TIGREtelescope obtaining intermediate-resolution spectra of R = 20,000. We appliedthe same method as described in our previous publication of this series. Forthe analysis of the radial velocity curves, we used the toolkit RadVel, whichallowed us to determine all orbital parameters. Recently published orbitalsolutions of some systems from Gaia DR3 agree with our results. However, oursolutions have much smaller uncertainties. We determined the basic stellarparameters of the primary stars with our automatic script using iSpec. Theparameter determination allowed us to place all nine stars in theHertzsprung-Russell diagram. We found that all stars have already evolved tothe giant phase. A comparison with stellar evolution tracks of the Eggletoncode was applied to determine the stellar masses and ages. As a result of ouranalysis, we were able to estimate the masses of the secondary stars and theorbital inclinations of the binary systems.

Bright Spectroscopic Binaries: III. Binary systems with orbital periods of P > 500 days