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• W2890350679 abstract "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 imaged orbiting a star. Thus it offers unique opportunities of detailed studies of its orbital, physical and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations from 2003 with NaCo at VLT, all following astrometric measurements relative to bpic have been obtained on the southwestern part, which severely limits the determination of the planet's orbital parameters. We aimed at further constraining bpic b orbital properties using more data, and, in particular data taken in the northeastern part of the orbit. We used the SPHERE instrument at VLT to precisely monitor the orbital motion of beta Pictoris b since 2014 (SPHERE first Light). We could monitor the planet until November 2016, when its too short angular separation (125 mas, i.e. 1.6,au) prevented further detection. We re-detected bpic b on the northeast side of the disk at a separation of 139,mas and a PA of 30$^{circ}$ in September 2018. The planet orbit is now well constrained. With a semi-major axis of $a = 9.0 pm 0.5$ (1 $sigma $), it definitely excludes previously reported possible long orbital periods, and excludes bpic b as the origin of the 1981 photometric event. We also refine the planet eccentricity and inclination. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters orbiting at less than 2 au from a star 20 pc away." @default.
• W2890350679 created "2018-09-27" @default.
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• W2890350679 date "2018-09-22" @default.
• W2890350679 modified "2023-10-14" @default.
• W2890350679 title "beta Pictoris b post conjunction detection with VLT/SPHERE" @default.
• W2890350679 hasPublicationYear "2018" @default.
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