The mass of β Pictoris c from β Pictoris b orbital motion

  title={The mass of $\beta$ Pictoris c from $\beta$ Pictoris b orbital motion},
  author={Sylvestre Lacour and J. J. Wang and Laetitia Rodet and M. Nowak and Jinyi Shangguan and Herv'e Beust and Anne-Marie Lagrange and Roberto Abuter and Ant{\'o}nio Amorim and Ruben Asensio-Torres and Myriam Benisty and J. P. Berger and Sarah C. Blunt and A. Boccaletti and Alexander J. Bohn and M. Bolzer and Micka{\"e}l Bonnefoy and Henri Bonnet and Guillaume Bourdarot and Walter Brandner and Faustine Cantalloube and Paola Caselli and Benjamin Charnay and Ga{\"e}l Chauvin and {\'E}lodie Choquet and Valentin Christiaens and Y. Cl'enet and Vincent Coud'e du Foresto and Alex J. Cridland and Roderick Dembet and Jason Dexter and P. T. de Zeeuw and Anderson Drescher and G. Duvert and Andreas Eckart and Frank Eisenhauer and Feng Gao and P. Garcia and Ram{\'o}n J. Garc{\'i}a L{\'o}pez and Eric Gendron and Reinhard Genzel and Stefan Gillessen and J. H. Girard and Xavier Haubois and Gernot Hei{\ss}el and T Henning and Sasha Hinkley and Stephen Hippler and M. Horrobin and M. Houll'e and Zolt{\'a}n Hubert and L. Jocou and Jens Kammerer and Miriam Keppler and P. Kervella and Laura Kreidberg and Vincent Lapeyr{\`e}re and J.-B. Le Bouquin and P. L'ena and Dieter Lutz and A.-L. Maire and Antoine M'erand and Paul Molli{\`e}re and John D. Monnier and David Mouillet and Evert Nasedkin and Thomas Ott and G. P. P. L. Otten and Claudia Paladini and T. Paumard and K. Perraut and Guy Perrin and Oliver Pfuhl and Emily L. Rickman and Laurent Pueyo and Julien Rameau and G. Rousset and Zafar Rustamkulov and Matthias Samland and Taro Shimizu and David K. Sing and J. Stadler and Tomas Stolker and Odele Straub and C. Straubmeier and Eckhard Sturm and L. J. Tacconi and Ewine F. van Dishoeck and Arthur Vigan and F. H. Vincent and S. D. von Fellenberg and K. Ward-Duong and Felix Widmann and Ekkehard Wieprecht and Erich Wiezorrek and Julien Woillez and S. Yazici and Alex Young and the Gravity Collaboration},
  journal={Astronomy \& Astrophysics},
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 b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations… 

Figures and Tables from this paper

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

N-body Interactions will be Detectable in the HR-8799 System within 5 yr with VLTI-GRAVITY

While Keplerian orbits account for the majority of the astrometric motion of directly-imaged planets, perturbations due to N-body interactions allow us to directly constrain exoplanet masses in

Stellar Obliquities in Exoplanetary Systems

The rotation of a star and the revolutions of its planets are not necessarily aligned. This article reviews the measurement techniques, key findings, and theoretical interpretations related to the

3D Selection of 167 Substellar Companions to Nearby Stars

We analyze 5108 AFGKM stars with at least five high-precision radial velocity points, as well as Gaia and Hipparcos astrometric data, utilizing a novel pipeline developed in previous work. We find

First Doppler Limits on Binary Planets and Exomoons in the HR 8799 System

We place the first constraints on binary planets and exomoons from Doppler monitoring of directly imaged exoplanets. We model radial velocity observations of HR 8799 b, c, and d from Ruffio et al.

The JWST Early Release Science Program for the Direct Imaging and Spectroscopy of Exoplanetary Systems

The direct characterization of exoplanetary systems with high-contrast imaging is among the highest priorities for the broader exoplanet community. As large space missions will be necessary for

Evolution of VLTI science operations: supporting imaging, astrometry, and monitoring types of interferometric observations

ESO’s VLT interferometer (VLTI) is a general-user optical/infrared interferometric facility. Its operations scheme is fully integrated into the well-established scheme of all VLT instruments and

The Pyxis Interferometer (I): scientific context, metrology system, and optical design

Optical interferometry from space is arguably the most exciting prospect for high angular resolution astrophysics; including the analysis of exoplanet atmospheres. This was highlighted in the recent

α-deep Probabilistic Inference (α-DPI): Efficient Uncertainty Quantification from Exoplanet Astrometry to Black Hole Feature Extraction

Inference is crucial in modern astronomical research, where hidden astrophysical features and patterns are often estimated from indirect and noisy measurements. Inferring the posterior of hidden



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

Evidence for an additional planet in the β Pictoris system

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

Dynamical Mass Estimates of the β Pictoris Planetary System through Gaussian Process Stellar Activity Modeling

Nearly 15 yr of radial velocity (RV) monitoring and direct imaging enabled the detection of two giant planets orbiting the young, nearby star β Pictoris. The δ Scuti pulsations of the star, which

A Model-independent Mass and Moderate Eccentricity for β Pic b

We use a cross-calibration of Hipparcos and Gaia second data release astrometry for β Pic to measure the mass of the giant planet β Pic b (13 ± 3 ) in a comprehensive joint orbit analysis that

Mean-Motion Resonances as a Source for Infalling Comets toward β Pictoris

Abstract Repeated time-variable redshifted absorption features in the spectrum of β Pictoris (β Pic) have been attributed to comet-like bodies falling toward the star, when evaporating in its

The First Dynamical Mass Measurement in the HR 8799 System

HR 8799 hosts four directly imaged giant planets, but none has a mass measured from first principles. We present the first dynamical mass measurement in this planetary system, finding that the

Constraining the Nature of the PDS 70 Protoplanets with VLTI/GRAVITY

We present K-band interferometric observations of the PDS 70 protoplanets along with their host star using VLTI/GRAVITY. We obtained K-band spectra and 100 μas precision astrometry of both PDS 70 b

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

Masses and Orbital Inclinations of Planets in the PSR B1257+12 System

We present measurements of the true masses and orbital inclinations of the two Earth-mass planets in the PSR B1257+12 system, based on the analysis of their mutual gravitational perturbations

Falling Evaporating Bodies as a Clue to Outline the Structure of the β Pictoris Young Planetary System

Transient redshifted events monitored in the spectrum offl Pictoris have been interpreted for many years as resulting from the evaporation of numerous comet-like bodies in the vicinity of this stars.