Radial velocity of TOI-201

We present the confirmation of the eccentric warm giant planet TOI-201b, first identified as a candidate in Transiting Exoplanet Survey Satellite photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using ground-based photometry from Next Generation Transit Survey and radial velocities from FEROS, HARPS, CORALIE, and Minerva-Australis. TOI-201b orbits a young (0.87_-0.49_^+0.46^Gyr) and bright (V=9.07mag) F-type star with a 52.9781day period.

The planet has a mass of 0.42_-0.03_^+0.05^M_J_, a radius of 1.008_-0.015_^+0.012^R_J_, and an orbital eccentricity of 0.28_-0.09_^+0.06^; 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-201b are important for constraining formation and evolution theories for giant planets.