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Context. The {\beta} Pictoris system with its debris disk and a massive giantplanet orbiting at \simeq 9 AU represents an ideal laboratory to study giantplanet formation and evolution as well as planet-disk interactions. {\beta} Picb can also help testing brightness-mass relations at young ages. Other planets,yet undetected, may of course be present in the system. Aims. We aim at puttingdirect constrains on the mass of {\beta} Pic b and at searching for additionaljovian planets on orbits closer than typically 2 AU. Methods. We use highprecision Harps data collected over 8 years since 2003 to measure and analyse{\beta} Pic radial velocities. Results. We show that the true mass of {\beta}Pic b is less than 10, 12, 15.5, 20 and 25 MJup if orbiting respectively at 8,9, 10, 11 and 12 AU. This is the first direct constraint on the mass of animaged planet. The upper mass found is well in the range predicted bybrightness-mass relations provided by current "hot start" models. We alsoexclude the presence of giant planets more massive than 2.5 MJup with periodsless than 100 days (hot Jupiters), more massive than 9 MJup for periods in therange 100-500 days. In the 500-1000 day range, the detection limit is in thebrown dwarf domain. Beyond the intrinsic interest for {\beta} Pic, theseresults show the possibilities of precise RV measurements of early type,rapidly rotating stars.

Constrains on planets around beta Pic with Harps radial velocity data