Post-conjunction detection of β Pictoris b with VLT/SPHERE

Lagrange, A.-M.; Boccaletti, A.; Langlois, M.; Chauvin, G.; Gratton, R.; Beust, H.; Desidera, S.; Milli, J.; Bonnefoy, M.; Cheetham, A.; Feldt, M.; Meyer, M.; Vigan, A.; Biller, B.; Bonavita, M.; Baudino, J.-L.; Cantalloube, F.; Cudel, M.; Daemgen, S.; Delorme, P.; ... (2019). Post-conjunction detection of β Pictoris b with VLT/SPHERE. Astronomy and astrophysics, 621, L8. EDP Sciences 10.1051/0004-6361/201834302

[img]
Preview
Text
1809.08354.pdf - Submitted Version
Available under License Creative Commons: Attribution (CC-BY).

Download (844kB) | Preview
[img]
Preview
Text
aa34302-18.pdf - Published Version
Available under License Creative Commons: Attribution (CC-BY).

Download (781kB) | Preview

With an orbital distance comparable to that of Saturn in the solar system, ß is the closest (semi-major axis ≃ 9 au) exoplanet that has been imaged to orbit a star. Thus it offers unique opportunities for detailed studies of its orbital, physical, and atmospheric properties, and of disk-planet interactions. With the exception of the discovery observations in 2003 with NaCo at the Very Large Telescope (VLT), all following astrometric measurements relative to ß have been obtained in the southwestern part of the orbit, which severely limits the determination of the planet's orbital parameters. We aimed at further constraining ß orbital properties using more data, and, in particular, data taken in the northeastern part of the orbit. We used SPHERE at the VLT to precisely monitor the orbital motion of beta ß since first light of the instrument in 2014. We were able to monitor the planet until November 2016, when its angular separation became too small (125 mas, i.e., 1.6 au) and prevented further detection. We redetected ß on the northeast side of the disk at a separation of 139\,mas and a PA of 30° in September 2018. The planetary orbit is now well constrained. With a semi-major axis (sma) of a=9.0±0.5 au (1 σ), it definitely excludes previously reported possible long orbital periods, and excludes ß as the origin of photometric variations that took place in 1981. We also refine the eccentricity and inclination of the planet. From an instrumental point of view, these data demonstrate that it is possible to detect, if they exist, young massive Jupiters that orbit at less than 2 au from a star that is 20 pc away.

Item Type:

Journal Article (Original Article)

Division/Institute:

08 Faculty of Science > Physics Institute > Space Research and Planetary Sciences > Theoretical Astrophysics and Planetary Science (TAPS)
08 Faculty of Science > Physics Institute > Space Research and Planetary Sciences
08 Faculty of Science > Physics Institute
08 Faculty of Science > Physics Institute > NCCR PlanetS

UniBE Contributor:

Mordasini, Christoph

Subjects:

500 Science
500 Science > 520 Astronomy
500 Science > 530 Physics
600 Technology > 620 Engineering

ISSN:

0004-6361

Publisher:

EDP Sciences

Language:

English

Submitter:

Janine Jungo

Date Deposited:

20 May 2019 18:18

Last Modified:

20 May 2019 18:18

Publisher DOI:

10.1051/0004-6361/201834302

ArXiv ID:

1809.08354v2

BORIS DOI:

10.7892/boris.128727

URI:

https://boris.unibe.ch/id/eprint/128727

Actions (login required)

Edit item Edit item
Provide Feedback