A Transiting Warm Giant Planet around the Young Active Star TOI-201
Name
Hobson_2021_AJ_161_235.pdf
Description
Published version
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Author(s)
Ricker, George R
Seager, Sara
Daylan, Tansu
Huang, Chelsea X.
Shporer, Abraham-Avi
Date Issued
2021
Journal
Astronomical Journal
Publisher
American Astronomical Society
Version
Final published version
Abstract
We present the confirmation of the eccentric warm giant planet TOI-201 b,
first identified as a candidate in \textit{TESS} photometry (Sectors 1-8,
10-13, and 27-28) and confirmed using ground-based photometry from NGTS and
radial velocities from FEROS, HARPS, CORALIE, and \textsc{Minerva}-Australis.
TOI-201 b orbits a young ($\mathrm{0.87^{+0.46}_{-0.49} \, Gyr}$) and
bright(V=9.07 mag) F-type star with a $\mathrm{52.9781 \, d}$ period. The
planet has a mass of $\mathrm{0.42^{+0.05}_{-0.03}\, M_J}$, a radius of
$\mathrm{1.008^{+0.012}_{-0.015}\, R_J}$, and an orbital eccentricity of
$0.28^{+0.06}_{-0.09}$; it appears to still be undergoing fairly rapid cooling,
as expected given the youth of the host star. The star also shows long-term
variability in both the radial velocities and several activity indicators,
which we attribute to stellar activity. The discovery and characterization of
warm giant planets such as TOI-201 b is important for constraining formation
and evolution theories for giant planets.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences
Massachusetts Institute of Technology. Department of Aeronautics and Astronautics
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Persistent DSpace Link
DOI of Published Version
https://doi.org/10.3847/1538-3881/ABEAA1
