TESS Hunt for Young and Maturing Exoplanets (THYME): a planet in the 45 Myr Tucana–Horologium association
Name
Newton_2019_ApJL_880_L17.pdf
Description
Published version
Size
1.88 MB
Format
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Author(s)
Newton, Elisabeth R.
Ricker, George R.
Vanderspek, Roland K.
Seager, Sara
Burke, Christopher J.
Fausnaugh, Michael
Villasenor, Jesus Noel Samonte
Villeneuva, Steven
Date Issued
July 2019
Journal
Astrophysical journal. Letters
Publisher
American Astronomical Society
Citation
Newton, Elisabeth R., et al., "TESS Hunt for Young and Maturing Exoplanets (THYME): a planet in the 45 Myr Tucana–Horologium association." Astrophysical journal. Letters 880, 1 (July 2019): letter 17 doi 10.3847/2041-8213/AB2988 ©2019 Author(s)
Version
Final published version
Abstract
Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana-Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from Southern Astrophysical Research/Goodman, South African Extremely Large Telescope/High Resolution Spectrograph and Las Cumbres Observatories/Network of Robotic Echelle Spectrographs; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/Gemini Planet Imager. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is 5.70 ± 0.17 R ⊕ and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15° to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V = 8.5) for detailed characterization using radial velocities and transmission spectroscopy. ©2019
MIT Department
Massachusetts Institute of Technology. Department of Physics
Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences
Massachusetts Institute of Technology. Department of Aeronautics and Astronautics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.3847/2041-8213/AB2988
