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.
Categories: astro-ph.EP