  The detection and characterization of exoplanets and brown dwarfs (BDs)
around massive AF-type stars is essential to investigate and constrain the
impact of stellar mass on planet properties. However, such targets are still
poorly explored in radial velocity (RV) surveys because they only feature a
small number of stellar lines and those are usually broadened and blended by
stellar rotation as well as stellar jitter. As a result, the available
information about the formation and evolution of planets and BDs around hot
stars is limited. We aim to increase the sample and precisely measure the
masses and eccentricities of giant planets and BDs transiting AF-type stars
detected by the Transiting Exoplanet Survey Satellite (TESS). We followed
bright (V < 12 mag) stars with $T_{\mathrm{eff}}$ > 6200 K that host giant
companions (R > 7 $\mathrm{R_{\rm \oplus}}$) using ground-based photometric
observations as well as high precision RV measurements from the CORALIE,
CHIRON, TRES, FEROS, and MINERVA-Australis spectrographs. In the context, we
present the discovery of three BD companions, TOI-629b, TOI-1982b, and
TOI-2543b, and one massive planet, TOI-1107b. From the joint analysis we find
the BDs have masses between 66 and 68 $\mathrm{M_{\rm Jup}}$, periods between
7.54 and 17.17 days, and radii between 0.95 and 1.11 $\mathrm{R_{\rm Jup}}$.
The hot Jupiter TOI-1107b has an orbital period of 4.08 days, a radius of 1.30
$\mathrm{R_{\rm Jup}}$, and a mass of 3.35 $\mathrm{M_{\rm Jup}}$. As a
by-product of this program, we identified four low-mass eclipsing components
(TOI-288b, TOI-446b, TOI-478b, and TOI-764b). Both TOI-1107b and TOI-1982b
present an anomalously inflated radius with respect to the age of these
systems. TOI-629 is among the hottest stars with a known transiting brown
dwarf. TOI-629b and TOI-1982b are among the most eccentric brown dwarfs.
