Abstract
AbstractIn 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, θ 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.
Highlights
From February 2015 until September 2020, a radial velocity ( ) monitoring campaign of selected binary systems was carried out at the University Observatory Jena, which is located close to the small village Großschwabhausen (Pfau, 1984)
The telescope is equipped with the fiber-linked Échelle spectrograph FLECHAS (Mugrauer, Avila, & Guirao, 2014)
The main part of our target sample are already published in Bischoff et al (2017) and Heyne et al (2020)
Summary
From February 2015 until September 2020, a radial velocity ( ) monitoring campaign of selected binary systems was carried out at the University Observatory Jena, which is located close to the small village Großschwabhausen (Pfau, 1984). The telescope is equipped with the fiber-linked Échelle spectrograph FLECHAS (Mugrauer, Avila, & Guirao, 2014). The aim of this campaign was to record data of spectroscopic binaries and to constrain or improve their orbital solutions. All targets from our original sample were chosen from the 9th Catalogue of Spectroscopic Binary Orbits (SB9 hereafter) from Pourbaix et al (2004). The SB9 catalogue is available in the VizieR1 database (Ochsenbein, Bauer, & Marcout, 2000) and contains information about orbital elements of several thousand spectroscopic binary stars. Cep had a grade of 1 and was suitable as a target for our observations. The orbital elements were taken from Abt (1961)
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