The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

Desidera, S.; Covino, E.; Messina, S.; Carson, J.; Hagelberg, J.; Schlieder, Joshua E.; Biazzo, K.; Alcalá, J. M.; Chauvin, G.; Vigan, A.; Beuzit, Jean-Luc; Bonavita, M.; Bonnefoy, M.; Delorme, P.; D’Orazi, V.; Esposito, M.; Feldt, M.; Girardi, L.; Gratton, R.; Henning, Thomas; Lagrange, Anne-Marie; Lanzafame, A. C.; Launhardt, R.; Marmier, M.; Melo, C.; Meyer, Michael; Mouillet, D.; Moutou, C.; Ségransan, D.; Udry, S.; Zaidi, C. M.

doi:10.1051/0004-6361/201323168

Cited by 93 publications

(109 citation statements)

References 221 publications

(322 reference statements)

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“…Then, we searched the SIMBAD/CDS databases (Wenger et al 2000) for radial velocity information using the data mining tools available on the site. The radial velocities that we use in this work come from Wilson (1953), Duflot et al (1995), Barbier-Brossat & Figon (2000), Torres et al (2006), Gontcharov (2006), Holmberg et al (2007), Mermilliod et al (2009), Chen et al (2011), Song et al (2012, Kordopatis et al (2013) and Desidera et al (2015). We found radial velocity for 184 stars of our sample.…”

Section: Appendix A: Ad Hoc Force To Account For Type II Migrationmentioning

confidence: 67%

Origin of the wide-orbit circumbinary giant planet HD 106906

Rodet

Beust

Bonnefoy

et al. 2017

A&A

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Context. A giant planet has been recently resolved at a projected distance of 730 au from the tight pair of young (∼13 Myr) intermediate-mass stars HD 106906AB in the Lower Centaurus Crux (LCC) group. The stars are surrounded by a debris disk which displays a ring-like morphology and strong asymmetries at multiple scales. Aims. We aim to study the likelihood of a scenario where the planet formed closer to the stars in the disk, underwent inward diskinduced migration, and got scattered away by the binary star before being stabilized by a close encounter (fly-by). Methods. We performed semi-analytical calculations and numerical simulations (Swift_HJS package) to model the interactions between the planet and the two stars. We accounted for the migration as a simple force. We studied the LCC kinematics to set constraints on the local density of stars, and therefore on the fly-by likelihood. We performed N-body simulations to determine the effects of the planet trajectories (ejection and secular effects) onto the disk morphology. Results. The combination of the migration and mean-motion resonances with the binary star (often 1:6) can eject the planet. Nonetheless, we estimate that the fly-by hypothesis decreases the scenario probability to less than 10 −7 for a derived local density of stars of 0.11 stars/pc 3 . We show that the concomitant effect of the planet and stars trajectories induce spiral-features in the disk which may correspond to the observed asymmetries. Moreover, the present disk shape suggests that the planet is on an eccentric orbit. Conclusions. The scenario we explored is a natural hypothesis if the planet formed within a disk. Conversely, its low probability of occurrence and the fact that HD 106906 b shares some characteristics with other systems in Sco-Cen (e.g., HIP 78530, in terms of mass ratio and separation) may indicate an alternative formation pathway for those objects.

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Section: Appendix A: Ad Hoc Force To Account For Type II Migrationmentioning

confidence: 67%

Origin of the wide-orbit circumbinary giant planet HD 106906

Rodet

Beust

Bonnefoy

et al. 2017

A&A

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“…The main objectives of these surveys were to populate the mass vs. semi-major axis diagram at large separations, and to clarify the mechanisms of planetary formation. Among the most recent of these surveys we can cite the NACO-Large Program at the Very Large Telescope (Desidera et al 2014;Chauvin et al 2014), the Strategic Exploration of Exoplanets and Disk with Subaru (SEEDS) at the Subaru Telescope (Janson et al 2013;Brandt et al 2014), the Near-Infrared Coronagraphic Imager (NICI) campaign at the Gemini South Telescope (Nielsen et al 2013;Biller et al 2013), the International Deep Planet Survey (Vigan et al 2012) at the Very Large Telescope (VLT) and Gemini North, and a survey of young, nearby, and dusty stars to understand the formation of wide-orbit giant planets (Rameau et al 2013b) at VLT.…”

Section: Introductionmentioning

confidence: 99%

Performance of the VLT Planet Finder SPHERE

Zurlo

Vigan

Mesa

et al. 2014

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Context. The new planet finder for the Very Large Telescope (VLT), the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), just had its first light in Paranal. A dedicated instrument for the direct detection of planets, SPHERE, is composed of a polametric camera in visible light, the Zurich IMager POLarimeter (ZIMPOL), and two near-infrared sub-systems: the Infra-Red Dual-beam Imager and Spectrograph (IRDIS), a multi-purpose camera for imaging, polarimetry, and long-slit spectroscopy, and the integral field spectrograph (IFS), an integral field spectrograph. Aims. We present the results obtained from the analysis of data taken during the laboratory integration and validation phase, after the injection of synthetic planets. Since no continuous field rotation could be performed in the laboratory, this analysis presents results obtained using reduction techniques that do not use the angular differential imaging (ADI) technique. Methods. To perform the simulations, we used the instrumental point spread function (PSF) and model spectra of L and T-type objects scaled in contrast with respect to the host star. We evaluated the expected error in astrometry and photometry as a function of the signal to noise of companions, after spectral differential imaging (SDI) reduction for IRDIS and spectral deconvolution (SD) or principal component analysis (PCA) data reductions for IFS. Results. We deduced from our analysis, for example, that β Picb, a 12 Myr old planet of ∼10 M Jup and semi-major axis of 9-10 AU, would be detected with IRDIS with a photometric error of 0.16 mag and with a relative astrometric position error of 1.1 mas. With IFS, we could retrieve a spectrum with error bars of about 0.15 mag on each channel and astrometric relative position error of 0.6 mas. For a fainter object such as HR 8799d, a 13 M Jup planet at a distance of 27 AU, IRDIS could obtain a relative astrometric error of 3 mas.

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“…J. Beuzit, Desidera et al 2015;Chauvin et al 2015), the work presented in this paper represents the first attempt to place some constraints on the full CMF in the substellar regime. It takes both BDs and planets into account and makes use of the results of most of the direct imaging surveys of solartype primaries currently available.…”

Section: Introductionmentioning

confidence: 84%

“…2 consisted of the targets of the NaCo-LP (Chauvin et al 2015;Desidera et al 2015), a large observing program (ESO: 184.C-0157) in the context of the VLT/SPHERE scientific preparation. This program is a direct imaging survey providing a homogeneous statistically significant study of the occurrence of giant planets and BDs in wide (5-500 AU) orbits around young, nearby stars.…”

Section: Datasetmentioning

confidence: 99%

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The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

Reggiani

Meyer

Chauvin

et al. 2016

A&A

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Context. In recent years there have been many attempts to characterize the occurrence and distribution of stellar, brown dwarf (BD), and planetary-mass companions to solar-type stars with the aim of constraining formation mechanisms. From radial velocity observations a dearth of companions with masses between 10-40 M Jupiter has been noticed at close separations, suggesting the possibility of a distinct formation mechanism for objects above and below this range. Aims. We present a model for the substellar companion mass function (CMF). This model consists of the superposition of the planet and BD companion mass distributions, assuming that we can extrapolate the radial velocity measured CMF for planets to larger separations and the stellar companion mass-ratio distribution over all separations into the BD mass regime. By using both the results of the VLT/NaCo large program (NaCo-LP) and the complementary archive datasets, which probe the occurrence of planets and BDs on wide orbits around solar-type stars, we place some constraints on the planet and BD distributions. Methods. We developed a Monte Carlo simulation tool to predict the outcome of a given survey, depending on the shape of the orbital parameter distributions (mass, semimajor axis, eccentricity, and inclination). Comparing the predictions with the results of the observations, we calculate the likelihood of different models and which models can be ruled out. Results. Current observations are consistent with the proposed model for the CMF, as long as a sufficiently small outer truncation radius ( 100 AU) is introduced for the planet separation distribution. Some regions of parameter space can be excluded by the observations. Conclusions. We conclude that the results of the direct imaging surveys searching for substellar companions around Sun-like stars are consistent with a combined substellar mass spectrum of planets and BDs. This mass distribution has a minimum between 10 and 50 M Jupiter , in agreement with radial velocity measurements. In this picture the dearth of objects in this mass range would naturally arise from the shape of the mass distribution, without the introduction of any distinct formation mechanism for BDs. This kind of model for the CMF allows us to determine the probability for a substellar companion as a function of mass to have formed in a disk or from protostellar core fragmentation, as such mechanisms overlap in this mass range.

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The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs in wide orbits

Cited by 93 publications

References 221 publications

Origin of the wide-orbit circumbinary giant planet HD 106906

Origin of the wide-orbit circumbinary giant planet HD 106906

Performance of the VLT Planet Finder SPHERE

The VLT/NaCo large program to probe the occurrence of exoplanets and brown dwarfs at wide orbits

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