Abstract
We present the latest results of an ongoing multiplicity survey of exoplanet hosts, which was initiated at the Astrophysical Institute and University Observatory Jena, using data from the second data release of the ESA-Gaia mission. In this study the multiplicity of 289 targets was investigated, all located within a distance of about 500 pc from the Sun. In total, 41 binary, and five hierarchical triple star systems with exoplanets were detected in the course of this project, yielding a multiplicity rate of the exoplanet hosts of about 16%. A total of 61 companions (47 stars, a white dwarf, and 13 brown dwarfs) were detected around the targets, whose equidistance and common proper motion with the exoplanet hosts were proven with their precise Gaia DR2 astrometry, which also agrees with the gravitational stability of most of these systems. The detected companions exhibit masses from about 0.016 up to 1.66 M⊙ and projected separations in the range between about 52 and 9,555 au.
Highlights
Since the detection of the first planet orbiting a star other than the Sun, several thousands of these exoplanets have been discovered by various detection techniques
which was initiated at the Astrophysical Institute
In order to explore the effects of the presence of stellar companions
Summary
Since the detection of the first planet orbiting a star other than the Sun, several thousands of these exoplanets have been discovered by various detection techniques. In order to clearly detect such companions and to prove the equidistance of these objects and the exoplanet hosts, in this study we have taken into account only Gaia DR2 sources with an accurate five parameter astrometric solution, i.e. which exhibit precise measurements of their parallax (π/σ(π) > 3) and proper motion (μ/σ(μ) > 3). The masses and effective temperatures of all detected companions were determined from their derived absolute G-band magnitudes using the evolutionary models of (sub)stellar objects from Baraffe et al (2015), as well as the ages of the exoplanet hosts, as listed in the EPE. I.e. the sum of the mass of the companions, derived as described above, and the mass of the associated exoplanet hosts, taken from the EPE This estimation can be considered as an upper limit of the escape velocity as the projected separation is smaller than the physical separation of the objects
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