  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.
