  In this paper, we carry out simulations of radial velocity (RV) measurements
of the mass of the 8-11 Myr Neptune-sized planet K2-33b using high-precision
near infrared velocimeters like SPIRou at the Canada-France-Hawaii Telescope.
We generate a RV curve containing a planet signature and a realistic stellar
activity signal, computed for a central wavelength of 1.8 $\mu$m and
statistically compatible with the light-curve obtained with K2. The modelled
activity signal includes the effect of time-evolving dark and bright surface
features hosting a 2 kG radial magnetic field, resulting in a RV signal of
semi-amplitude ~30 m/s. Assuming a 3-month visibility window, we build RV
time-series including Gaussian white noise from which we retrieve the planet
mass while filtering the stellar activity signal using Gaussian Process
Regression. We find that 35/50 visits spread over 3 consecutive bright-time
runs on K2-33 allow one to reliably detect planet RV signatures of respectively
10 and 5 m/s at precisions larger than 3 $\sigma$. We also show that 30 visits
may end up being insufficient in some cases to provide a good coverage of the
stellar rotation cycle, with the result that the planet signature can go
undetected or the mass estimation be plagued by large errors.
