The AstraLux Binary M Dwarfs Survey

Bergfors, C.; Brandner, W.; Hippler, S.; Henning, Thomas; Janson, Markus; Hormuth, F.

doi:10.1017/s1743921311028080

Cited by 1 publication

(1 citation statement)

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“…Consequently, there is a real need to characterize the orbital properties of recently imaged EGPs, to determine the planetary system architectures and dynamical stabilities, and to obtain additional constraints on their formation and evolution mechanisms. Follow-up astrometric studies have been conducted on the HR 8799 multiple exoplanetary system (Lafrenière et al 2009;Marois et al 2010;Bergfors et al 2011;Soummer et al 2011). Inclined orbital solutions for the b and d planets, and a 1:2:4 resonance for the planets c, d, and e, confirm stable configurations supported by dynamical simulations (Reidemeister et al 2009 Murray-Clay 2010).…”

Section: Introductionmentioning

confidence: 84%

Orbital characterization of the βPictoris b giant planet

Chauvin,

Lagrange,

Beust

et al. 2012

Preprint

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Context. In June 2010, we confirmed the existence of a giant planet in the disk of the young star β Pictoris located between 8 AU and 15 AU from the star. This young planet offers the rare opportunity to monitor a large fraction of the orbit using the imaging technique over a reasonably short timescale. It also offers the opportunity to study its atmospheric properties using spectroscopy and multi-band photometry, and possibly derive its dynamical mass by combining imaging with radial velocity data to set tight constraints on giant planet formation theories. Aims. We aim to measure the evolution of the planet's position relative to the star β Pictoris to determine the planetary orbital properties. Our ultimate goal is to relate both the planetary orbital configuration and physical properties to either the disk structure or the cometary activity observed for decades in the β Pictoris system. Methods. Using the NAOS-CONICA adaptive-optics instrument (NACO) at the Very Large Telescope (VLT), we obtained repeated follow-up images of the β Pictoris system in the Ks and L ′ filters at four new epochs in 2010 and 2011. Complementing these data with previous measurements, we conduct a homogeneous analysis, which covers more than eight yrs, to accurately monitor the β Pictoris b position relative to the star. Results. On the basis of the evolution of the planet's relative position with time, we derive the best-fit orbital solutions for our measurements. More reliable results are found with a Markov-chain Monte Carlo approach. The solutions favor a low-eccentricity orbit e < ∼ 0.17, with semi-major axis in the range 8-9 AU corresponding to orbital periods of 17-21 yrs. Our solutions favor a highly inclined solution with a peak around i = 88.5 ± 1.7 o , and a longitude of ascending node tightly constrained at Ω = −147.5 ± 1.5 • . These results indicate that the orbital plane of the planet is likely to be above the midplane of the main disk, and compatible with the warp component of the disk being tilted between 3.5 deg and 4.0 deg. This suggests that the planet plays a key role in the origin of the inner warped-disk morphology of the β Pic disk. Finally, these orbital parameters are consistent with the hypothesis that the planet is responsible for the transit-like event observed in November 1981, and also linked to the cometary activity observed in the β Pic system. Conclusions.

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