The orbit of beta Pictoris b as a transiting planet

@article{tangs2016TheOO,
  title={The orbit of beta Pictoris b as a transiting planet},
  author={A. Lecavelier des {\'E}tangs and Alfred Vidal-Madjar},
  journal={Astronomy and Astrophysics},
  year={2016},
  volume={588}
}
In 1981, Beta Pictoris showed strong and rapid photometric variations possibly due to a transiting giant planet. Later, a planetary mass companion to the star, Beta Pic b, was identified using imagery. Observations at different epochs (2003 and 2009-2015) detected the planet at a projected distance of 6 to 9 AU from the star and showed that the planet is on an edge-on orbit. The observed motion is consistent with an inferior conjunction in 1981, and Beta Pic b can be the transiting planet… 

Figures and Tables from this paper

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

Context. With an orbital distance comparable to that of Saturn in the solar system, β Pictoris b is the closest (semi-major axis ≃9 au) exoplanet that has been imaged to orbit a star. Thus it offers

Search for rings and satellites around the exoplanet CoRoT-9b using Spitzer photometry

Using Spitzer photometry at 4.5 microns, we search for rings and satellites around the long period transiting planet CoRoT-9b. We observed two transits in 2010 and 2011. From their non-detection, we

The slow spin of the young sub-stellar companion GQ Lupi b and its orbital configuration

The spin of a planet or brown dwarf is related to the accretion process, and therefore studying spin can help promote our understanding of the formation of such objects. We present the projected

bRing: An observatory dedicated to monitoring the $\beta$ Pictoris b Hill sphere transit

Aims. We describe the design and first light observations from the $\beta$ Pictoris b Ring ("bRing") project. The primary goal is to detect photometric variability from the young star $\beta$

THE ORBIT AND TRANSIT PROSPECTS FOR β PICTORIS b CONSTRAINED WITH ONE MILLIARCSECOND ASTROMETRY

A principal scientific goal of the Gemini Planet Imager (GPI) is obtaining milliarcsecond astrometry to constrain exoplanet orbits. However, astrometry of directly imaged exoplanets is subject to

ALMA Resolves C i Emission from the β Pictoris Debris Disk

The debris disk around β Pictoris is known to contain gas. Previous ALMA observations revealed a CO belt at ∼85 au with a distinct clump, interpreted as a location of enhanced gas production.

Characterizing exo-ring systems around fast-rotating stars using the Rossiter–McLaughlin effect

Planetary rings produce a distinct shape distortion in transit lightcurves. However, to accurately model such lightcurves the observations need to cover the entire transit, especially ingress and

β Pictoris: observations of the Ca ii H&K absorptions in 1997 and 1998

We present spectroscopy with resolution R ∼ 33 000 of the circumstellar Ca ii H&K absorptions in the star β Pictoris during 1997 and 1998. From 1997 April onwards, both lines were observed

The δ Scuti pulsations of β Pictoris as observed by ASTEP from Antarctica

Aims. The Antarctica Search for Transiting Extrasolar Planets (ASTEP), an automatized 400 mm telescope located at Concordia station in Antarctica, monitored β Pictoris continuously to detect any

Reaching sub-milimag photometric precision on Beta Pictoris with a nanosat: the PicSat mission

PicSat is a nanosatellite currently being developed to observe the transit of the giant planet β Pictoris, expected some time between July 2017 and June 2018. The mission is based on a Cubesat

References

SHOWING 1-10 OF 37 REFERENCES

Is Beta Pic b the transiting planet of November 1981

In 1981, Beta Pictoris showed strong and rapid photometric variations that were attributed to the transit of a giant comet or a planet orbiting at several AUs (Lecavelier des Etangs et al. 1994,

Orbital characterization of the β Pictoris b giant planet

In June 2010, we confirmed the existence of a giant planet in the disk of the young star Beta Pictoris, located between 8 AU and 15 AU from the star. This young planet offers the rare opportunity to

Constraining the orbit of the possible companion to Beta Pictoris: New deep imaging observations

We recently reported on the detection of a possible planetary-mass companion to Beta Pictoris at a projected separation of 8 AU from the star, using data taken in November 2003 with NaCo, the

THE GEMINI NICI PLANET-FINDING CAMPAIGN: THE ORBIT OF THE YOUNG EXOPLANET β PICTORIS b

We present new astrometry for the young (12–21 Myr) exoplanet β Pictoris b taken with the Gemini/NICI and Magellan/MagAO instruments between 2009 and 2012. The high dynamic range of our observations

Fast spin of the young extrasolar planet β Pictoris b

The combined line profile exhibits a rotational broadening of about 25 kilometres per second, meaning that β Pictoris b spins significantly faster than any planet in the Solar System, in line with the extrapolation of the known trend in spin velocity with planet mass.

A posteriori detection of the planetary transit of HD 189733 b in the Hipparcos photometry

Aims. Using observations performed at the Haute-Provence Observatory, the detection of a 2.2-day orbital period extra-solar planet that transits the disk of its parent star, HD 189733, has been

The fast spin-rotation of a young extrasolar planet

The spin-rotation of a planet arises from the accretion of angular momentum during its formation, but the details of this process are still unclear. In the solar system, the equatorial rotation

The near-infrared spectral energy distribution of β Pictoris b

A gas giant planet has previously been directly seen orbiting at 8-10 AU within the debris disk of the ~12 Myr old star {\beta} Pictoris. The {\beta} Pictoris system offers the rare opportunity to

β Pictoris, a young planetary system? A review

Optical Images of an Exosolar Planet 25 Light-Years from Earth

Optical observations of an exoplanet candidate, Fomalhaut b, show that the planet's mass is at most three times that of Jupiter; a higher mass would lead to gravitational disruption of the belt, matching predictions of its location.