TOI-1259Ab – a gas giant planet with 2.7 per cent deep transits and a bound white dwarf companion

Creators: Martin, David V.; El-Badry, Kareem; Kunovac Hodžić, Vedad; Triaud, Amaury H. M. J.; Angus, Ruth; Birky, Jessica L.; Foreman-Mackey, Daniel; Hedges, Christina; Montet, Benjamin T.; Murphy, Simon J.; Santerne, Alexandre; Stassun, Keivan G.; Stephan, Alexander P.; Wang, Ji; Benni, Paul; Krushinsky, Vadim; Chazov, Nikita; Mishevskiy, Nikolay; Ziegler, Carl; Soubkiou, Abderahmane; Benkhaldoun, Zouhair; Boisse, Isabelle; Battley, Matthew; Miller, Nicola J.; Caldwell, Douglas A.; Collins, Karen; Henze, Christopher E.; Guerrero, Natalia M.; Jenkins, Jon M.; Latham, David W.; Levine, Adam; McDermott, Scott; Mullally, Susan E.; Ricker, George; Seager, Sara; Shporer, Avi; Vanderburg, Andrew; Vanderspek, Roland; Winn, Joshua N.

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Abstract

We present TOI-1259Ab, a 1.0 R_(Jup) gas giant planet transiting a 0.71 R_⊙ K-dwarf on a 3.48 d orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of ∼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 m s⁻¹⁠, implying a planet mass of 0.44 M_(Jup). By fitting the spectral energy distribution of the white dwarf, we derive a total age of 4.08^(+1.21)_(−0.53) Gyr for the system. The K dwarf's 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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© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). This project began at the Expanding the Science of TESS meeting, which took place in 2020 February the University of Sydney, back when meeting people in large groups was still a thing. The RV observations were partly conducted while OHP was in 'remote observing' mode, a special mode produced as a response the unique COVID-19 situation. We are extremely grateful for the dedication of the staff at OHP that allowed observations to resume. We thank Markus Mugrauer for looking at a draft version of this paper. Finally, we thank a referee for providing a thorough review that undoubtedly improved the quality of the paper. The observations were obtained under an OHP DDT programme (PI Triaud). This work was in part funded by the U.S.–Norway Fulbright Foundation and a NASA TESS GI grant G022253 (PI: Martin). DVM received funding from the Swiss National Science Foundation (grant P 400P2 186735). AHMJT received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant 803193/BEBOP). VKH is also supported by a Birmingham Doctoral Scholarship, and by a studentship from Birmingham's School of Physics & Astronomy. SG has been supported by STFC through consolidated grants ST/L000733/1 and ST/P000495/1. SJM was supported by the Australian Research Council through DECRA DE180101104. VK has been supported by the Ministry of science and Higher Education of the Russian Federation , topic № FEUZ-2020-0038. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS SPOC. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has used AstroPy,8 a community-developed core python package for Astronomy (Astropy Collaboration 2013, 2018). Based in part on observations made at Observatoire de Haute Provence (CNRS), France. DATA AVAILABILITY. All TESS data are publicaly available and can be downloaded using lightkurve (Lightkurve Collaboration 2018) or other tools. The SOPHIE RVs are published as supplementary data. Any other data/models in this article will be shared on reasonable request to the corresponding author.

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Resource type: Journal Article
Publisher: Royal Astronomical Society
Published in: Monthly Notices of the Royal Astronomical Society, 507(3), 4132-4148, ISSN: 0035-8711.