Evidence for an additional planet in the β Pictoris system

Lagrange, Anne-Marie; Meunier, N.; Rubini, P.; Keppler, M.; Galland, F.; Chapellier, E.; Michel, E.; Balona, L. A.; Beust, H.; Guillot, T.; Grandjean, A.; Borgniet, S.; Mékarnia, D.; Wilson, Paul; Kiefer, F.; Bonnefoy, M.; Lillo-Box, J.; Pantoja, B.; Jones, M. I.; Iglesias, Daniela; Rodet, L.; Díaz, Matías R.; Zapata, A.; Abe, Lyu; Schmider, F. X.

doi:10.1038/s41550-019-0857-1

Cited by 97 publications

(105 citation statements)

References 34 publications

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“…Similarly to Lagrange et al (2019), we find the presence of the c planet results in a lower mass for the b planet. In our one-planet Case 3 fit, we found a mass for β Pic b of M b = 12.8 +5.5 −3.2 M Jup , which drops to M b = 8.0 ± 2.6 M Jup in the coplanar fit ( Figure 17).…”

supporting

confidence: 67%

“…Compared to Lagrange et al (2019), we find generally similar values to our fit, but with noticeable differences, likely resulting from performing a joint fit for all data and both planets, rather than using MCMC chains from a fit to β Pic b to fit the RVs. Lagrange et al (2019) found values of [a c , e c , P c , M c ] of [2.69 ± 0.003 au, 0.24 ± 0.02, 3.335 ± 0.005 yr, 8.93 ± 0.14 M Jup ] compared to values from our coplanar fit of [2.72 ± 0.019 au, 0.24 +0.1 −0.09 , 3.39 ± 0.02 yr, 9.18 +1.0 −0.9 M Jup ]. That these measurements are in such good agreement, but with errors several times larger from the joint fit, suggests that extracting a limited number of orbits from the posterior, as done in Lagrange et al (2019), underestimates the errors on the derived parameters.…”

supporting

confidence: 66%

“…After this paper was submitted, Lagrange et al (2019) presented radial velocity measurements of β Pic and an orbit fit for an inner giant planet, β Pic c, orbiting at 2.7 au. In particular, by fitting for the δ Scuti pulsations of the star, they were able to detect the ∼4 year signal of the inner planet.…”

Section: Comparison To Previous Orbit Fitsmentioning

confidence: 99%

“…Despite having no constraint on mutual inclination, the inclination angle and position angle of nodes for c (i c and Ω c ) differ from the priors, and follow the orbit of β Pic b, but with larger uncertainties: i b = 88.8 ± 1.0 • and Ω b = 32.02 ± 0.08 • for the outer planet, compared to Figure 15. Posteriors from the fit to Case 3 and the stellar RVs from Lagrange et al (2019), including a second planet (β Pic c), with no additional constraints on mutual inclination between the two planets.…”

Section: Comparison To Previous Orbit Fitsmentioning

confidence: 99%

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The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry

Nielsen

Rosa

Wang

et al. 2020

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We present new observations of the planet β Pictoris b from 2018 with GPI, the first GPI observations following conjunction. Based on these new measurements, we perform a joint orbit fit to the available relative astrometry from ground-based imaging, the Hipparcos Intermediate Astrometric Data (IAD), and the Gaia DR2 position, and demonstrate how to incorporate the IAD into direct imaging orbit fits. We find a mass consistent with predictions of hot-start evolutionary models and previous works following similar methods, though with larger uncertainties: 12.8 +5.3 −3.2 M Jup . Our eccentricity determination of 0.12 +0.04 −0.03 disfavors circular orbits. We consider orbit fits to several different imaging datasets, and find generally similar posteriors on the mass for each combination of imaging data. Our analysis underscores the importance of performing joint fits to the absolute and relative astrometry simultaneously, given the strong covariance between orbital elements. Time of conjunction is well constrained within 2.8 days of 2017 September 13, with the star behind the planet's Hill sphere between 2017 April 11 and 2018 February 16 (± 18 days). Following the recent radial velocity detection of a second planet in the system, β Pic c, we perform additional two-planet fits combining relative astrometry, absolute astrometry, and stellar radial velocities. These joint fits find a significantly smaller mass for the imaged planet β Pic b, of 8.0 ± 2.6 M Jup , in a somewhat more circular orbit. We expect future ground-based observations to further constrain the visual orbit and mass of the planet in advance of the release of Gaia DR4.

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supporting

confidence: 67%

supporting

confidence: 66%

Section: Comparison To Previous Orbit Fitsmentioning

confidence: 99%

Section: Comparison To Previous Orbit Fitsmentioning

confidence: 99%

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The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry

Nielsen

Rosa

Wang

et al. 2020

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“…Indeed, our immediate Galactic environment is richly populated with stars that harbour planetary systems. We are already aware of many stars with known exoplanets within only a few parsecs around the Sun, such as for example, Proxima Centauri at 1.3 pc (Anglada-Escudé et al 2016), Barnard's Star at 1.8 pc (Ribas et al 2018), Teegarden's Star at 3.8 pc (Zechmeister et al 2019), Fomalhaut at 7.7 pc (Kalas et al 2008) 2 , Trappist-1 at 12 pc (Gillon et al 2017), or β Pictoris at 19 pc (Lagrange et al , 2019. Most stars in Sun-like environments 3 seem to host planets.…”

Section: Introductionmentioning

confidence: 99%

ISPY-NACO Imaging Survey for Planets around Young stars

Launhardt

Henning

Quirrenbach

et al. 2020

A&A

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Context. The occurrence rate of long-period (a 50 au) giant planets around young stars is highly uncertain since it is not only governed by the protoplanetary disc structure and planet formation process, but also reflects both dynamical re-structuring processes after planet formation as well as possible capture of planets not formed in situ. Direct imaging is currently the only feasible method to detect such wide-orbit planets and constrain their occurrence rate. Aims. We aim to detect and characterise wide-orbit giant planets during and shortly after their formation phase within protoplanetary and debris discs around nearby young stars. Methods. We carry out a large L -band high-contrast direct imaging survey for giant planets around 200 young stars with protoplanetary or debris discs using the NACO instrument at the ESO Very Large Telescope on Cerro Paranal in Chile. We use very deep angular differential imaging observations with typically >60 • field rotation, and employ a vector vortex coronagraph where feasible to achieve the best possible point source sensitivity down to an inner working angle of about 100 mas. This paper introduces the NACO Imaging Survey for Planets around Young stars (NACO-ISPY), its goals and strategy, the target list, and data reduction scheme, and presents preliminary results from the first 2.5 survey years. Results. We achieve a mean 5 σ contrast of ∆L = 6.4 ± 0.1 mag at 150 mas and a background limit of L bg = 16.5 ± 0.2 mag at >1. 5. Our detection probability is >50% for companions with 8 M Jup at semi-major axes of 80-200 au and >13 M Jup at 30-250 au. It thus compares well to the detection space of other state-of-the-art high-contrast imaging surveys. We have already contributed to the characterisation of two new planets originally discovered by VLT/SPHERE, but we have not yet independently discovered new planets around any of our target stars. We have discovered two new close-in low-mass stellar companions around R CrA and HD 193571 and report in this paper the discovery of close co-moving low-mass stellar companions around HD 72660 and HD 92536. Furthermore, we report L -band scattered light images of the discs around eleven stars, six of which have never been imaged at L -band before. Conclusions. The first 2.5 yr of the NACO-ISPY survey have already demonstrated that VLT/NACO combined with our survey strategy can achieve the anticipated sensitivity to detect giant planets and reveal new close stellar companions around our target stars.

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Detecting life outside our solar system with a large high-contrast-imaging mission

et al. 2021

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In this White Paper, which was submitted in response to the European Space Agency (ESA) Voyage 2050 Call, we recommend the ESA plays a proactive role in developing a global collaborative effort to construct a large high-contrast imaging space telescope, e.g. as currently under study by NASA. Such a mission will be needed to characterize a sizable sample of temperate Earth-like planets in the habitable zones of nearby Sun-like stars and to search for extraterrestrial biological activity. We provide an overview of relevant European expertise, and advocate ESA to start a technology development program towards detecting life outside the Solar System.

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Evidence for an additional planet in the β Pictoris system

Cited by 97 publications

References 34 publications

The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry

The Gemini Planet Imager Exoplanet Survey: Dynamical Mass of the Exoplanet β Pictoris b from Combined Direct Imaging and Astrometry

ISPY-NACO Imaging Survey for Planets around Young stars

Detecting life outside our solar system with a large high-contrast-imaging mission

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