Kavli Affiliate: Sara Seager
| First 5 Authors: Ján Šubjak, David W. Latham, Samuel N. Quinn, Perry Berlind, Michael L. Calkins
| Summary:
The present study reports the confirmation of BD-14 3065b, a transiting
planet/brown dwarf in a triple-star system, with a mass near the deuterium
burning boundary. BD-14 3065b has the largest radius observed within the sample
of giant planets and brown dwarfs around post-main-sequence stars. Its orbital
period is 4.3 days, and it transits a subgiant F-type star with a mass of
$M_star=1.41 pm 0.05 M_{odot}$, a radius of $R_star=2.35 pm 0.08
R_{odot}$, an effective temperature of $T_{rm eff}=6935pm90$ K, and a
metallicity of $-0.34pm0.05$ dex. By combining TESS photometry with
high-resolution spectra acquired with the TRES and Pucheros+ spectrographs, we
measured a mass of $M_p=12.37pm0.92 M_J$ and a radius of $R_p=1.926pm0.094
R_J$. Our discussion of potential processes that could be responsible for the
inflated radius led us to conclude that deuterium burning is a plausible
explanation resulting from the heating of BD-14 3065b’s interior. Detection of
the secondary eclipse with TESS photometry enables a precise determination of
the eccentricity $e_p=0.066pm0.011$ and reveals BD-14 3065b has a brightness
temperature of $3520 pm 130$ K. With its unique characteristics, BD-14 3065b
presents an excellent opportunity to study its atmosphere through thermal
emission spectroscopy.
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