Since early 2015, a new radial velocity monitoring campaign is going on at the University Observatory Jena. The aim of this project is to obtain current radial velocity measurements of selected single‐lined spectroscopic binary systems as well as to redetermine and/or constrain their orbital solutions. In this paper, we characterize the properties of the target sample of the project, describe the spectroscopic observations, data reduction, and analysis, and present the first results of the project, taken with the fiber‐linked astronomical spectrograph FLECHAS. We present 391 radial velocity measurements of eight spectroscopic binaries, which were taken within an epoch difference of 1.6 years. These radial velocities were used to determine the spectroscopic orbital elements of the observed binary systems, which exhibit orbital periods in the range between nearly one up to several dozens of days. We could constrain the orbital solutions of seven of these binary systems, and redetermine the orbital solution of φ Dra, whose orbit exhibits >4 times longer orbital period and is more eccentric than given in the 9th Catalogue of Spectroscopic Binary Orbits.

We present the results of our second radial velocity (RV) monitoring campaign, carried out with the Échelle spectrograph FLECHAS at the University Observatory Jena in the course of the Großschwabhausen binary survey between December 2016 and June 2018. The aim of this project is to obtain precise RV measurements for spectroscopic binary stars in order to redetermine, verify, improve, and constrain their Keplerian orbital solutions. In this paper, we describe the observations, data reduction, and analysis and present the results of this project. In total, we have taken 721 RV measurements of 11 stars and derived well‐determined orbital solutions for nine systems (seven single‐ and two double‐lined spectroscopic binaries) with periods in the range between 2 and 70 days. In addition, we could rule out the orbital solutions for the previously classified spectroscopic binary systems HIP 107136 and HIP 107533, whose radial velocities are found to be constant on the km s−1‐level over a span of time of more than 500 days. In the case of HIP 2225, a significant change of its systematic velocity is detected between our individual observing epochs, indicating the presence of an additional companion, which is located on a wider orbit in this system.

In 2015, a radial velocity monitoring campaign was started in order to redetermine and/or constrain the orbital solutions of spectroscopic binary systems. The observations were carried out at the University Observatory Jena with the Échelle spectrograph FLECHAS. The results from the main part of our target sample are already published. For the final target of this campaign, Cep, we can now present an orbital solution based on a homogeneously covered radial velocity curve. The period of this single-lined spectroscopic binary turned out to be significantly larger, and the orbit is much more eccentric compared to the given values in the 9th Catalogue of Spectroscopic Binary Orbits.

We present the results of our spectroscopic monitoring observations of the late O‐type runaway stars AE Aur and ι Ori, carried out between September 2016 and May 2018 using the Échelle spectrograph FLECHAS at the University Observatory Jena. For both stars, we obtained current radial velocity (RV) measurements with better precision than before. These results can be used for further advanced calculations of their space motion, needed to determine, for example, their place of origin in our Galaxy. In this paper, we describe the observations and the data reduction, as well as the analysis of all spectral data. We find a stable RV for AE Aur and confirm ι Ori as a double‐lined spectroscopic binary and derive its current Keplerian orbital elements.