http://arxiv.org/abs/2103.02685
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.
M. Hobson, R. Brahm, A. Jordán, et. al.
Fri, 5 Mar 21
42/64
Comments: 21 pages, 11 figures, accepted to AJ
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