The 14 Her Planetary System: Companion Masses and Architecture from Radial Velocities and Astrometry

Abstract

We combine Hubble Space Telescope (HST) Fine Guidance Sensor, Hipparcos, and Gaia DR3 astrometric observations of the K0 V star 14 Her with the results of an analysis of extensive ground-based radial velocity data to determine perturbation orbits and masses for two previously known companions, 14 Her b and c. Radial velocities obtained with the Hobby–Eberly Telescope and from the literature now span over 25 years. With these data we obtain improved radial velocity (RV) orbital elements for both the inner companion, 14 Her b and the long-period outer companion, 14 Her c. We also find evidence of an additional RV signal with P ∼ 3789 ^d . We then model astrometry from Hipparcos, HST, and Gaia with RV results to obtain system parallax and proper motion, perturbation periods, inclinations, and sizes due to 14 Her b and c. We find P _b = 1767.6 ± 0.2 days, perturbation semimajor axis α _b = 1.3 ± 0.1 mas, and inclination i _b = 36° ± 3°, P _c = 52160 ± 1028 days, perturbation semimajor axis α _c = 10.3 ± 0.7 mas, and inclination i _c = 82° ± 14°. In agreement with a past investigation, the 14 Her b, c orbits exhibit significant mutual inclination. Assuming a primary mass M _* = 0.98 ± 0.04 M _☉ , we obtain companion masses ${{ \mathcal M }}_{{\rm{b}}}={8.5}_{-0.8}^{+1.0}$ ${{ \mathcal M }}_{\mathrm{Jup}}\,$ and ${{ \mathcal M }}_{{\rm{c}}}={7.1}_{-0.6}^{+1.0}$ ${{ \mathcal M }}_{\mathrm{Jup}}$ .

Keywords

• Exoplanets