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With an orbital distance comparable to that of Saturn in the solar system,\bpic b is the closest (semi-major axis $\simeq$\,9\,au) exoplanet that hasbeen imaged to orbit a star. Thus it offers unique opportunities for detailedstudies of its orbital, physical, and atmospheric properties, and ofdisk-planet interactions. With the exception of the discovery observations in2003 with NaCo at the Very Large Telescope (VLT), all following astrometricmeasurements relative to \bpic have been obtained in the southwestern part ofthe orbit, which severely limits the determination of the planet's orbitalparameters. We aimed at further constraining \bpic b orbital properties usingmore data, and, in particular, data taken in the northeastern part of theorbit.  We used SPHERE at the VLT to precisely monitor the orbital motion of beta\bpic b since first light of the instrument in 2014. We were able to monitorthe planet until November 2016, when its angular separation became too small(125 mas, i.e., 1.6\,au) and prevented further detection. We redetected \bpic bon the northeast side of the disk at a separation of 139\,mas and a PA of30$^{\circ}$ in September 2018. The planetary orbit is now well constrained.With a semi-major axis (sma) of $a = 9.0 \pm 0.5$ au (1 $\sigma $), itdefinitely excludes previously reported possible long orbital periods, andexcludes \bpic b as the origin of photometric variations that took place in1981. We also refine the eccentricity and inclination of the planet. From aninstrumental point of view, these data demonstrate that it is possible todetect, if they exist, young massive Jupiters that orbit at less than 2 au froma star that is 20 pc away.

Post conjunction detection of $\beta$ Pictoris b with VLT/SPHERE