  Our aim is to detect and characterise long-period companions around main
sequence stars (spectral types late F to early M). We use the RV method to
search for exoplanets around stars. The RV variations are measured with HARPS
at the ESO 3.6 metre telescope. The true mass and inclination of our heavier
companions are provided by astrometry, for which we use proper motions from
Hipparcos and Gaia. Five Jupiter-mass exoplanets are reported to orbit
HIP54597, BD-210397 (x2), HD74698, and HD94771 with 8.9 yr, 5.2 yr, 17.4 yr,
9.4 yr, and 5.9 yr orbits, and to have minimum masses of $2.01 \pm 0.03$, $0.7
\pm 0.1$, $2.4^{+1.5}_{-0.2}$, $0.40 \pm 0.06$, and $0.53 \pm 0.03 M_J$
respectively. HD74698 also hosts a highly irradiated Neptune in a 15 day orbit
with a minimum mass of $0.07 \pm 0.01 M_J$. The mass of HIP54597 b can
maximally increase by 10% - 30%, the minimum mass of HD74698 c is likely equal
to its true mass, and BD-210397 c has a mass of $2.66^{+0.63}_{-0.32} M_J$.
HD62364 hosts a brown dwarf with a true mass of $18.77^{+0.66}_{-0.63} M_J$ in
an orbit of 14 yr. HD56380B, HD221638B, and HD33473C have minimum masses within
the brown dwarf limits, in orbits of 8.9 yr, 16.6 yr, and 50 yr respectively;
however, astrometric measurements reveal them to be stellar binaries, with
masses of $375.3^{+8.6}_{-8.4}$, $110.0^{+3.9}_{-3.7}$, and
$271.0^{+3.9}_{-3.8} M_J$. The orbits of the stellar binaries HD11938 and
HD61383 are incomplete. The preliminary result for HD61383 is a 0.190
$M_{\odot}$ binary in a 39 yr orbit. The secondary of the binary system HD11938
has a mass of 0.33 $M_{\odot}$ - which is confirmed by a secondary peak in the
CCF - and a preliminary period of 35 yr. The origin of the 3.0 yr RV signal of
HD3964 is uncertain as it shows entanglement with the magnetic cycle of the
star. We finally report one more star, HD11608, with a magnetic cycle that
mimics a planetary signal.
