We report the discovery and characterization of two sub-Saturns from the Transiting Exoplanet Survey Satellite (TESS) using high-resolution spectroscopic observations from the MaHPS spectrograph at the Wendelstein Observatory and the SOPHIE spectrograph at the Haute-Provence Observatory. Combining photometry from TESS, KeplerCam, LCOGT, and MuSCAT2 with the radial velocity measurements from MaHPS and SOPHIE we measure precise radii and masses for both planets. TOI-5108 b is a sub-Saturn with a radius of 6.6+/-0.1R_{Earth}_ and a mass of 32+/-5M_{Earth}_ TOI-5786 b is similar to Saturn with a radius of 8.63+/-0.12R_{Earth}_ and a mass of 72+/-8M_{Earth}_. Both planets are close to their host stars with periods of 6.75 days and 12.78 days respectively. This puts TOI-5108 b just inside the bounds of the Neptune desert while TOI-5786 b is right above the upper edge. We estimate hydrogen-helium envelope mass fractions of 38% for TOI-5108 b and 74% for TOI-5786 b. However, using a model for the interior structure that includes tidal effects the envelope fraction of TOI-5108 b could be much lower (~20$) depending on the obliquity. We estimate mass-loss rates between 1.0x10^9^g/s and 9.8x10^9^g/s for TOI-5108 b and between 3.6x10^8^g/s and 3.5x10^9^g/s for TOI-5786 b. Given their masses, this means that both planets are stable against photoevaporation. Furthermore, at these mass-loss rates, there is likely no detectable signal in the metastable helium triplet with the James Webb Space Telescope. We also detect a transit signal for a second planet candidate around TOI-5786 with a period of 6.998 days and a radius of 3.90+/-0.16R_{Earth}_ Using our RV data and photodynamical modeling, we are able to provide a 3-{sigma} upper limit of 26.5M_{Earth}_ for the mass of the potential inner companion to TOI-5786 b.