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The Transiting Exoplanet Survey Satellite (TESS) provides a continuous suiteof new planet candidates that need confirmation and precise mass determinationfrom ground-based observatories. This is the case for the G-type star TOI-1710,which is known to host a transiting sub-Saturn planet($\mathrm{M_p}=$28.3$\pm$4.7$\mathrm{M}_\oplus$) in a long-period orbit(P=24.28\,d). Here we combine archival SOPHIE and new and archival HARPS-Nradial velocity data with newly available TESS data to refine the planetaryparameters of the system and derive a new mass measurement for the transitingplanet, taking into account the impact of the stellar activity on the massmeasurement. We report for TOI-1710b a radius of$\mathrm{R_p}$$=$5.15$\pm$0.12$\mathrm{R}_\oplus$, a mass of$\mathrm{M_p}$$=$18.4$\pm$4.5$\mathrm{M}_\oplus$, and a mean bulk density of$\rho_{\rm p}$$=$0.73$\pm$0.18$\mathrm{g \, cm^{-3}}$, which are consistent at1.2$\sigma$, 1.5$\sigma$, and 0.7$\sigma$, respectively, with previousmeasurements. Although there is not a significant difference in the final massmeasurement, we needed to add a Gaussian process component to successfully fitthe radial velocity dataset. This work illustrates that adding moremeasurements does not necessarily imply a better mass determination in terms ofprecision, even though they contribute to increasing our full understanding ofthe system. Furthermore, TOI-1710b joins an intriguing class of planets withradii in the range 4-8 $\mathrm{R}_\oplus$ that have no counterparts in theSolar System. A large gaseous envelope and a bright host star make TOI-1710b avery suitable candidate for follow-up atmospheric characterization.

Revisiting the warm sub-Saturn TOI-1710b