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Spectroscopy of TOI-1259B – an unpolluted white dwarf companion to an inflated warm Saturn

Evan FitzmauriceDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, Columbus, OH 43210, USADavid V. MartinCenter for Cosmology and AstroParticle Physics, The Ohio State University , Columbus, OH 43210, USARomy Rodríguez MartínezDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, Columbus, OH 43210, USAPatrick J. VallelyCenter for Astrophysics | Harvard & Smithsonian , 60 Garden St, Cambridge, MA 02138, USAAlexander P. StephanDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, Columbus, OH 43210, USAKiersten M. BoleyCenter for Astrophysics | Harvard & Smithsonian , 60 Garden St, Cambridge, MA 02138, USARichard W. PoggeDepartment of Astronomy, The Ohio State University , 4055 McPherson Laboratory, Columbus, OH 43210, USAKareem El-BadrySchool of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, UKVedad KunovacLowell Observatory , 1400 W. Mars Hill Rd., Flagstaff, AZ 86001, USAA. H. M. J. TriaudSchool of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, UK

2022en

ABI

Annotatsiya

ABSTRACT TOI-1259 consists of a transiting exoplanet orbiting a main-sequence star, with a bound outer white dwarf (WDs) companion. Less than a dozen systems with this architecture are known. We conduct follow-up spectroscopy on the WD TOI-1259B using the Large Binocular Telescope to better characterize it. We observe only strong hydrogen lines, making TOI-1259B a DA WD. We see no evidence of heavy element pollution, which would have been evidence of planetary material around the WD. Such pollution is seen in $\sim 25{-}50{{\ \rm per\ cent}}$ of WDs, but it is unknown if this rate is higher or lower in TOI-1259-like systems that contain a known planet. Our spectroscopy permits an improved WD age measurement of $4.05^{+1.00}_{-0.42}$ Gyr, which matches gyrochronology of the main-sequence star. This is the first of an expanded sample of similar binaries that will allow us to calibrate these dating methods and provide a new perspective on planets in binaries.

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DOI: 10.1093/mnras/stac2879

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