LBT observations of the HR 8799 planetary system

Esposito, Simone; Mesa, D.; Skemer, Andrew J.; Arcidiacono, Carmelo; Claudi, R.; Desidera, S.; Gratton, R.; Mannucci, F.; Marzari, F.; Masciadri, E.; Close, Laird M.; Hinz, Philip M.; Kulesa, Craig; McCarthy, D. W.; Males, Jared R.; Agapito, Guido; Argomedo, Javier; Boutsia, K.; Briguglio, Runa; Brusa, Guido; Busoni, Lorenzo; Cresci, G.; Fini, Luca; Fontana, A.; Guerra, Juan Carlos; Hill, John M.; Miller, Doris I.; Paris, D.; Pinna, Enrico; Puglisi, Alfio; Quirós-Pacheco, Fernando; Riccardi, Armando; Stefanini, P.; Testa, V.; Xompero, Marco; Woodward, C. E.

doi:10.1051/0004-6361/201219212

Cited by 68 publications

(90 citation statements)

References 57 publications

(81 reference statements)

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“…Dynamical stability studies of the planetary system that orbits HR 8799 provide additional indirect evidence for a young system age. An older stellar age implied larger planet masses that would lead to a dynamically unstable system (Currie et al 2011;Sudol & Haghighipour 2012;Esposito et al 2013). Therefore, we adopt a value of 30 Myr for Tucana, Columba, and Carina and 45 Myr for Argus (the mean between isochrone and lithium depletion boundary ages).…”

Section: Tucana Columba Carina and Argusmentioning

confidence: 99%

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

Desidera

Covino

Messina

et al. 2015

A&A

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Context. Young, close stars are ideal targets for searching planets using the direct imaging technique. The determination of stellar parameters is crucial for the interpretation of imaging survey results, particularly since the luminosity of substellar objects has a strong dependence on system age. Aims. We have conducted a large program with NaCo at the VLT to search for planets and brown dwarfs in wide orbits around 86 stars. A large fraction of the targets observed with NaCo were poorly investigated in the literature. We performed a study to characterize the fundamental properties (age, distance, and mass) of the stars in our sample. To improve target age determinations, we compiled and analyzed a complete set of age diagnostics. Methods. We measured spectroscopic parameters and age diagnostics using dedicated observations acquired with FEROS and CORALIE spectrographs at La Silla Observatory. We also made extensive use of archival spectroscopic data and the results that are available in the literature. Additionally, we exploited photometric time-series, which are available in ASAS and Super-WASP archives, to derive a rotational period for a large fraction of our program stars. Results. We provided updated characterization of all the targets observed in the VLT NaCo Large program, a survey designed to probe the occurrence of exoplanets and brown dwarfs in wide orbits. The median distance and age of our program stars are 64 pc and 100 Myr, respectively. Nearly all the stars have masses between 0.70 and 1.50 M , with a median value of 1.01 M . The typical metallicity is close to solar with a dispersion that is smaller than that of samples usually observed in radial velocity surveys. Several stars are confirmed or proposed here to be members of close young moving groups. Eight spectroscopic binaries are identified.

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Section: Tucana Columba Carina and Argusmentioning

confidence: 99%

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

Desidera

Covino

Messina

et al. 2015

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“…The range will be shifted towards higher masses when assuming older ages. However, constraints from the stellar properties (Marois et al 2008;Baines et al 2012), the mass of the disk (Su et al 2009), and models of dynamical stability of the four planets (Esposito et al 2013;Goździewski & Migaszewski 2014) suggest that the system is young. Other hints for small radii or low masses of the planets come from the fitting of their spectral energy distribution (e.g., Marois et al 2008;Bowler et al 2010;Currie et al 2011;Barman et al 2011;Madhusudhan et al 2011;Galicher et al 2011;Ingraham et al 2014), although there are uncertainties on the atmospheric composition and the physical processes governing their atmospheres assumed for the models (e.g., solar/non-solar metallicity, physics of the clouds, non-equilibrium chemistry).…”

Section: Constraints On the Properties Of A Fifth Planetmentioning

confidence: 99%

“…The dotted line in the panel for HR 8799 e indicates the orbital solution labeled "B" in Table 5. The orange circles indicate the ephemeris predicted in Goździewski & Migaszewski (2014). and coplanar orbits (Goździewski & Migaszewski 2009Fabrycky & Murray-Clay 2010;Soummer et al 2011) and circular and non-coplanar orbits (Esposito et al 2013). Recently, Goździewski & Migaszewski (2014) have built a long-term stable model of the system, with all planets on quasi-circular coplanar orbits and likely involved in 8b:4c:2d:1e mean motion resonance.…”

Section: Orbital Architecturementioning

confidence: 99%

“…We first tested the predictions of Goździewski & Migaszewski (2014) with respect to the astrometric measurements presented in this paper. We gathered all the relative astrometric measurements available in the literature (Marois et al 2008(Marois et al , 2010bLafrenière et al 2009;Fukagawa et al 2009;Metchev et al 2009;Hinz et al 2010;Currie et al 2011Currie et al , 2012Currie et al , 2014Bergfors et al 2011;Galicher et al 2011;Soummer et al 2011;Esposito et al 2013;Pueyo et al 2015) and included the LEECH measurements (Table 2) to represent Fig. 3.…”

Section: Orbital Architecturementioning

confidence: 99%

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The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

Maire

Skemer

Hinz

et al. 2015

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Context. Astrometric monitoring of directly imaged exoplanets allows the study of their orbital parameters and system architectures. Because most directly imaged planets have long orbital periods (>20 AU), accurate astrometry is challenging when based on data acquired on timescales of a few years and usually with different instruments. The LMIRCam camera on the Large Binocular Telescope is being used for the LBT Exozodi Exoplanet Common Hunt (LEECH) survey to search for and characterize young and adolescent exoplanets in L band (3.8 µm), including their system architectures. Aims. We first aim to provide a good astrometric calibration of LMIRCam. Then, we derive new astrometry, test the predictions of the orbital model of 8:4:2:1 mean motion resonance proposed for the system, and perform new orbital fitting of the HR 8799 bcde planets. We also present deep limits on a putative fifth planet inside the known planets. Methods. We use observations of HR 8799 and the Θ 1 Ori C field obtained during the same run in October 2013. Results. We first characterize the distortion of LMIRCam. We determine a platescale and a true north orientation for the images of 10.707 ± 0.012 mas/pix and −0.430 ± 0.076 • , respectively. The errors on the platescale and true north orientation translate into astrometric accuracies at a separation of 1 of 1.1 mas and 1.3 mas, respectively. The measurements for all planets agree within 3σ with a predicted ephemeris. The orbital fitting based on the new astrometric measurements favors an architecture for the planetary system based on 8:4:2:1 mean motion resonance. The detection limits allow us to exclude a fifth planet slightly brighter or more massive than HR 8799 b at the location of the 2:1 resonance with HR 8799 e (∼9.5 AU) and about twice as bright as HR 8799 cde at the location of the 3:1 resonance with HR 8799 e (∼7.5 AU).

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“…Moreover, this technique allows us to obtain photometric, spectroscopic, and astrometric measurements of the detected companions, and for this reason it is a fundamental technique to study the atmosphere of the known objects, their mass-luminosity function and their orbits (see, e.g, Rameau et al 2013a;Kuzuhara et al 2013;Esposito et al 2013;Currie et al 2013) . However, direct detection of extrasolar planets is challenging for two reasons: (1) the large luminosity contrast with respect to the star, which is of the order of 10 −6 for giant young planets with high intrinsic luminosity, and 10 −8 -10 −9 for old planets seen in reflected and intrinsic light; and (2) the small separation between the star and the planet, of the order of a few tenths of arcsec for planets at few AUs around stars at a distance up to 100 pc from the Sun.…”

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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LBT observations of the HR 8799 planetary system

Cited by 68 publications

References 57 publications

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

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

The LEECH Exoplanet Imaging Survey. Further constraints on the planet architecture of the HR 8799 system

Performance of the VLT Planet Finder SPHERE

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