Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 507, Issue 3, Pages 4132-4148Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab2129
Keywords
planets and satellites: formation; binaries: eclipsing; stars: individual (TOI-1259); stars: low-mass; stars: rotation
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Funding
- U.S.-Norway Fulbright Foundation
- NASA TESS GI grant [G022253]
- Swiss National Science [P 400P2 186735]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [803193/BEBOP]
- Birmingham Doctoral Scholarship
- Birmingham's School of Physics Astronomy
- STFC [ST/L000733/1, ST/P000495/1]
- Australian Research Council through DECRA [DE180101104]
- Ministry of science and Higher Education of the Russian Federation [FEUZ2020-0038]
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TOI-1259Ab is a gas giant planet orbiting a K-dwarf, with a white dwarf companion in its system. Its deep transits make it a promising target for atmospheric characterization. By analyzing the age of the system through various measurements, there is consistency in the estimated total age.
We present TOI-1259Ab, a 1.0R(Jup) gas giant planet transiting a 0.71R(circle dot) K-dwarf on a 3.48d orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of similar to 1600 au from the planet host. Transits are observed in nine TESS sectors and are 2.7 per cent deep - among the deepest known - making TOI-1259Ab a promising target for atmospheric characterization. Our follow-up radial velocity measurements indicate a variability of semiamplitude K = 71 ms(-1), implying a planet mass of 0.44M(Jup). By fitting the spectral energy distribution of the white dwarf, we derive a total age of 4.08(-0.53)(+1.21) Gyr for the system. The K dwarfs light curve reveals rotational variability with a period of 28 d, which implies a gyrochronology age broadly consistent with the white dwarf's total age.
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