Context. HD113337 is a Main-Sequence F6V field star more massive than the Sun. It hosts one confirmed giant planet and possibly a second, candidate one, detected by radial velocities. It also hosts a cold debris disk detected through the presence of an infrared excess, making it an interesting system to explore. Aims. We aim at bringing new constraints on the star’s fundamental parameters, the debris disk properties and the planetary companion(s) by combining complementary techniques. Methods. We used the VEGA interferometer on the CHARA array to measure HD113337 angular diameter. We derived its linear radius using the parallax from Gaia Second Data Release. We computed the bolometric flux to derive its effective temperature and luminosity, and we estimated its mass and age using evolutionary tracks. Then, we used Herschel images to partially resolve the outer debris disk and estimate its extension and inclination. Next, we acquired high-contrast images of HD113337 with the LBTI to probe the ∼10-80 au separation range. Finally, we combined the deduced contrast maps with previous radial velocity (RV) of the star using the MESS2 software to bring upper mass limits on possible companions at all separations up to 80 au. We took advantage of the constraints on the age and inclination (brought by the fundamental parameter analysis and the disk imaging, respectively) for this analysis. Results. We derive a limb-darkened angular diameter of 0.386 ± 0.009 mas that converts into a linear radius of 1.50 ± 0.04 R for HD113337. The fundamental parameter analysis leads to an effective temperature of 6774 ± 125 K, and to two possible age solutions: one young within 14-21 Myr and one old within 0.8-1.7 Gyr. We partially resolve the known outer debris disk and model its emission. Our best solution corresponds to a radius of 85 ± 20 au, an extension of 30 ± 20 au and an inclination within 10-30◦ for the outer disk. The combination of imaging contrast limits, published RV, and age and inclination solutions allow us to derive a first possible estimation of the true masses of the planetary companions: ∼ 7+−42 MJup for HD113337 b (confirmed companion), and ∼ 16+−103 MJup for HD113337 c (candidate companion). We also constrain possible additional companions at larger separations.
|Original language||English (US)|
|State||Published - May 27 2019|
- Fundamental parameters
- High angular resolution – Stars: individual: HD113337
- Planetary systems
- Techniques: interferometric
ASJC Scopus subject areas