  We report the results of an extended spectropolarimetric and photometric
monitoring of the weak-line T Tauri star TAP 26, carried out within the MaTYSSE
programme with the ESPaDOnS spectropolarimeter at the 3.6 m
Canada-France-Hawaii Telescope. Applying Zeeman-Doppler Imaging to our
observations, concentrating in 2015 November and 2016 January and spanning 72 d
in total, 16 d in 2015 November and 13 d in 2016 January, we reconstruct
surface brightness and magnetic field maps for both epochs and demonstrate that
both distributions exhibit temporal evolution not explained by differential
rotation alone. We report the detection of a hot Jupiter (hJ) around TAP 26
using three different methods, two using Zeeman-Doppler Imaging (ZDI) and one
Gaussian-Process Regression (GPR), with a false-alarm probability smaller than
6.10^-4. However, as a result of the aliasing related to the observing window,
the orbital period cannot be uniquely determined; the orbital period with
highest likelihood is 10.79 +/- 0.14 d followed by 8.99 +/- 0.09 d. Assuming
the most likely period, and that the planet orbits in the stellar equatorial
plane, we obtain that the planet has a minimum mass M.sin(i) of 1.66 +/- 0.31
M_Jup and orbits at 0.0968 +/- 0.0032 au from its host star. This new detection
suggests that disc type II migration is efficient at generating newborn hJs,
and that hJs may be more frequent around young T Tauri stars than around mature
stars (or that the MaTYSSE sample is biased towards hJ-hosting stars).
