Evidence for an additional planet in the β Pictoris system

  title={Evidence for an additional planet in the $\beta$ Pictoris system},
  author={Anne-Marie Lagrange and Nad{\`e}ge Meunier and Pascal Rubini and Miriam Keppler and Franck Galland and Eric Chapellier and Eric Michel and Luis A. Balona and Herv'e Beust and Tristan Guillot and Antoine Grandjean and Simon Borgniet and Djamel M{\'e}karnia and Paul A Wilson and Flavien Kiefer and Micka{\"e}l Bonnefoy and Jorge Lillo-Box and Blake Pantoja and Mat'ias I. Jones and Daniela Iglesias and Laetitia Rodet and Mat{\'i}as R. D{\'i}az and Abner Zapata and Lyu Abe and François-Xavier Schmider},
  journal={Nature Astronomy},
With its imaged debris disk of dust, its evaporating exocomets, and an imaged giant planet, the young (~23 Myr) β Pictoris system is a unique proxy for detailed studies of planet formation processes as well as planet–disk interactions. Here, we study ten years of European Southern Observatory/High Accuracy Radial Velocity Planet Searcher (HARPS) high-resolution spectroscopic data of β Pictoris. After removing the radial velocity (RV) signals arising from the δ Scuti pulsations of the star, a ~1… 
The far reaches of the β Pictoris debris disk
The nearby young star beta Pictoris hosts a rich and complex planetary system, with at least two giant planets and a nearly edge-on debris disk that contains several dynamical subpopulations of
Unveiling the β Pictoris system, coupling high contrast imaging, interferometric, and radial velocity data
Context. The nearby and young β Pictoris system hosts a well resolved disk, a directly imaged massive giant planet orbiting at ≃9 au, as well as an inner planet orbiting at ≃2.7 au, which was
Peering into the formation history of β Pictoris b with VLTI/GRAVITY long-baseline interferometry
Context. β Pictoris is arguably one of the most studied stellar systems outside of our own. Some 30 yr of observations have revealed a highly-structured circumstellar disk, with rings, belts, and a
Spin–Orbit Alignment of the β Pictoris Planetary System
A crucial diagnostic that can tell us about processes involved in the formation and dynamical evolutionof planetary systems is the angle between the rotation axis of a star and a planet's orbital
Debris Disks in Multiplanet Systems: Are Our Inferences Compromised by Unseen Planets?
Resolved debris disk features (e.g., warps, offsets, edges and gaps, azimuthal asymmetries, radially thickened rings, scale heights) contain valuable information about the underlying planetary
Direct confirmation of the radial-velocity planetβPictoris c
Context.Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas
The mass of β Pictoris c from β Pictoris b orbital motion
Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris
Dynamical Mass of the Exoplanet Host Star HR 8799
HR 8799 is a young A5/F0 star hosting four directly imaged giant planets at wide separations (∼16–78 au), which are undergoing orbital motion and have been continuously monitored with adaptive optics
E P ] 2 8 A pr 2 02 2 Exocomets size distribution in the β Pictoris planetary system
The star β Pictoris harbors a young planetary system, which is characterized by the presence of a gaseous and dusty debris disk1–6, at least two massive planets7–10 and many minor bodies. For more


Constraints on planets around β Pic with Harps radial velocity data
Context. The β Pictoris system with its debris disk and a massive giant planet orbiting at � 9 AU represents an ideal laboratory for studying giant planet formation and evolution as well as
The mass of the young planet Beta Pictoris b through the astrometric motion of its host star
The young massive Jupiters discovered with high-contrast imaging1–4 provide a unique opportunity to study the formation and early evolution of gas giant planets. A key question is to what extent
A Giant Planet Imaged in the Disk of the Young Star β Pictoris
It is shown that the ~10-million-year-oldβ Pictoris system hosts a massive giant planet, β Pictoris b, located 8 to 15 astronomical units from the star, which confirms that gas giant planets form rapidly within disks and validates the use of disk structures as fingerprints of embedded planets.
The position of β Pictoris b position relative to the debris disk
Context. We detected in 2009 a giant, close-by planet orbiting β Pic, a young star surrounded by a disk that has been extensively studied for more than 20 years. We showed that if the planet were
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
A probable giant planet imaged in the beta Pictoris disk. VLT/NaCo deep L'-band imaging
Context: Since the discovery of its dusty disk in 1984, β Pictoris has become the prototype of young early-type planetary systems, and there are now various indications that a massive Jovian planet
Full exploration of the giant planet population around β Pictoris
Context. The search for extrasolar planets has been limited so far to close orbit (typ. ≤5 au) planets around mature solar-type stars on the one hand, and to planets on wide orbits (≥10 au) around
Dust depletion in the inner disk of β Pictoris as a possible indicator of planets
IT is not yet possible to see planets orbiting other stars, although this may soon change as observing methods improve1. Indirect evidence for the presence of circumstellar dust disks out of which
Mid-infrared images of β Pictoris and the possible role of planetesimal collisions in the central disk
Thermal infrared images of the central disk imply that the brightness asymmetry results from the presence of a bright clump composed of particles that may differ in size from dust elsewhere in the disk, which is suggested to result from the collisional grinding of resonantly trapped planetesimals or the cataclysmic break-up of a planetesimal.
Dynamical modeling of large scale asymmetries in the beta Pictoris dust disk
We report a new and complete model of the Pictoris disk, which succeeds in accounting for both the surface brightness distribution, warp characteristics, the outer \butterfly" asymmetry as observed