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

Maire, Anne-Lise; Skemer, Andrew J.; Hinz, Philip M.; Desidera, S.; Esposito, Simone; Gratton, R.; Marzari, F.; Skrutskie, M. F.; Biller, Beth; Defrère, Denis; Bailey, Vanessa P.; Leisenring, Jarron; Apai, Dániel; Bonnefoy, M.; Brandner, W.; Buenzli, E.; Claudi, R.; Close, Laird M.; Crepp, Justin R.; Rosa, Robert J. De; Eisner, J. A.; Fortney, Jonathan J.; Henning, Thomas; Hofmann, Karl H.; Kopytova, T.; Males, Jared R.; Mesa, D.; Morzinski, Katie M.; Oza, A.; Patience, Jennifer; Pinna, Enrico; Rajan, Abhijith; Schertl, D.; Schlieder, Joshua E.; Su, K. Y. L.; Vaz, Amali; Ward-Duong, Kimberly; Weigelt, G.; Woodward, C. E.

doi:10.1051/0004-6361/201425185

Cited by 64 publications

(68 citation statements)

References 78 publications

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“…The LBTI Exozodi Exoplanet Common Hunt (LEECH) is a ∼100-night survey with the Large Binocular Telescope (LBT) to search for and characterize exoplanets in the mid-infrared (Skemer et al 2014a;Maire et al 2015). In this work, we confirm the detection of GJ 504 band obtain photometry of the first T-dwarf exoplanet in three narrow L-band filters (3.71, 3.88, and 4.00 μm).…”

Section: Introductionsupporting

confidence: 68%

THE LEECH EXOPLANET IMAGING SURVEY: CHARACTERIZATION OF THE COLDEST DIRECTLY IMAGED EXOPLANET, GJ 504 b, AND EVIDENCE FOR SUPERSTELLAR METALLICITY*

Skemer

Morley

Zimmerman

et al. 2016

ApJ

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As gas giant planets and brown dwarfs radiate away the residual heat from their formation, they cool through a spectral type transition from L to T, which encompasses the dissipation of cloud opacity and the appearance of strong methane absorption. While there are hundreds of known T-type brown dwarfs, the first generation of directly imaged exoplanets were all Ltype. Recently, Kuzuhara et al. announced the discovery of GJ 504 b, the first T dwarf exoplanet. GJ 504 b provides a unique opportunity to study the atmosphere of a new type of exoplanet with a ∼500 K temperature that bridges the gap between the first directly imaged planets (∼1000 K) and our own solar systemʼs Jupiter (∼130 K). We observed GJ 504 b in three narrow L-band filters (3.71, 3.88, and 4.00 μm), spanning the red end of the broad methane fundamental absorption feature (3.3 μm) as part of the LBTI Exozodi Exoplanet Common Hunt (LEECH) exoplanet imaging survey. By comparing our new photometry and literature photometry with a grid of custom model atmospheres, we were able to fit GJ 504 bʼs unusual spectral energy distribution for the first time. We find that GJ 504 b is wellfit by models with the following parameters:.12, cloud opacity parameter of f sed =2-5, R=0.96±0.07 R Jup , and log(L)=−6.13±0.03 L e , implying a hot start mass of 3-30 M jup for a conservative age range of 0.1-6.5 Gyr. Of particular interest, our model fits suggest that GJ 504 b has a superstellar metallicity. Since planet formation can create objects with nonstellar metallicities, while binary star formation cannot, this result suggests that GJ 504 b formed like a planet, not like a binary companion.

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Section: Introductionsupporting

confidence: 68%

THE LEECH EXOPLANET IMAGING SURVEY: CHARACTERIZATION OF THE COLDEST DIRECTLY IMAGED EXOPLANET, GJ 504 b, AND EVIDENCE FOR SUPERSTELLAR METALLICITY*

Skemer

Morley

Zimmerman

et al. 2016

ApJ

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“…The sensitivity and utility of the LBTAO coupled with LBTI/LMIRcam has been demonstrated in several studies of known, substellar companions and a very low-mass binary (Skemer et al 2012(Skemer et al , 2014bBonnefoy et al 2014;Schlieder et al 2014). These capabilities also led to strong constraints on the possibility of a fifth planet in the HR 8799 planetary system during the LEECH survey (Maire et al 2015). Further technical details of the LEECH survey, including H and L′ contrast curves, are provided in Skemer et al (2014a).…”

Section: The Lbt Interferometer (Lbti) Exozodi Exoplanet Common Hunt mentioning

confidence: 99%

THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

Schlieder

Skemer

Maire

et al. 2016

ApJ

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We present high-resolution Large Binocular Telescope LBTI/LMIRcam images of the spectroscopic and astrometric binary NO UMa obtained as part of the LBT Interferometer Exozodi Exoplanet Common Hunt exoplanet imaging survey. Our H-, K s -, and L′-band observations resolve the system at angular separations <0 09. The components exhibit significant orbital motion over a span of ∼7 months. We combine our imaging data with archival images, published speckle interferometry measurements, and existing spectroscopic velocity data to solve the full orbital solution and estimate component masses. The masses of the K2.0±0.5 primary and K6.5±0.5 secondary are 0.83±0.02 M e and 0.64±0.02 M e , respectively. We also derive a system distance of d=25.87±0.02 pc and revise the Galactic kinematics of NO UMa. Our revised Galactic kinematics confirm NO UMa as a nuclear member of the ∼500 Myr old Ursa Major moving group, and it is thus a mass and age benchmark. We compare the masses of the NO UMa binary components to those predicted by five sets of stellar evolution models at the age of the Ursa Major group. We find excellent agreement between our measured masses and model predictions with little systematic scatter between the models. NO UMa joins the short list of nearby, bright, late-type binaries having known ages and fully characterized orbits.

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“…The uncertainties on the parameters were estimated using a quadratic combination of statistical and systematic errors. The statistical errors stem from the sensitivity of the fit to the errors bars on the astrometric measurements and are derived from 1000 random trials of the astrometric measurements assuming normal distributions (Maire et al 2015). The systematic errors are related to the uncertainties on the stellar mass and distance (Table 7), which propagate into the derivation of the semimajor axis.…”

Section: Astrometric Fit Of the Orbitsmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Zurlo

Vigan

Galicher

et al. 2016

A&A

Self Cite

146

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Context. The planetary system discovered around the young A-type HR 8799 provides a unique laboratory to: a) test planet formation theories; b) probe the diversity of system architectures at these separations, and c) perform comparative (exo)planetology. Aims. We present and exploit new near-infrared images and integral-field spectra of the four gas giants surrounding HR 8799 obtained with SPHERE, the new planet finder instrument at the Very Large Telescope, during the commissioning and science verification phase of the instrument (July-December 2014). With these new data, we contribute to completing the spectral energy distribution (SED) of these bodies in the 1.0-2.5 µm range. We also provide new astrometric data, in particular for planet e, to further constrain the orbits. Methods. We used the infrared dual-band imager and spectrograph (IRDIS) subsystem to obtain pupil-stabilized, dual-band H2H3 (1.593 µm, 1.667 µm), K1K2 (2.110 µm, 2.251 µm), and broadband J (1.245 µm) images of the four planets. IRDIS was operated in parallel with the integral field spectrograph (IFS) of SPHERE to collect low-resolution (R ∼ 30), near-infrared (0.94-1.64 µm) spectra of the two innermost planets HR 8799 d and e. The data were reduced with dedicated algorithms, such as the Karhunen-Loève image projection (KLIP), to reveal the planets. We used the so-called negative planets injection technique to extract their photometry, spectra, and measure their positions. We illustrate the astrometric performance of SPHERE through sample orbital fits compatible with SPHERE and literature data. Results. We demonstrated the ability of SPHERE to detect and characterize planets in this kind of systems, providing spectra and photometry of its components. The spectra improve upon the signal-to-noise ratio of previously obtained data and increase the spectral coverage down to the Y band. In addition, we provide the first detection of planet e in the J band. Astrometric positions for planets HR 8799 bcde are reported for the epochs of July, August, and December 2014. We measured the photometric values in J, H2H3, K1K2 bands for the four planets with a mean accuracy of 0.13 mag. We found upper limit constraints on the mass of a possible planet f of 3-7 M Jup . Our new measurements are more consistent with the two inner planets d and e being in a 2d:1e or 3d:2e resonance. The spectra of HR 8799 d and e are well matched by those of L6-8 field dwarfs. However, the SEDs of these objects are redder than field L dwarfs longward of 1.6 µm.

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

Cited by 64 publications

References 78 publications

THE LEECH EXOPLANET IMAGING SURVEY: CHARACTERIZATION OF THE COLDEST DIRECTLY IMAGED EXOPLANET, GJ 504 b, AND EVIDENCE FOR SUPERSTELLAR METALLICITY*

THE LEECH EXOPLANET IMAGING SURVEY: CHARACTERIZATION OF THE COLDEST DIRECTLY IMAGED EXOPLANET, GJ 504 b, AND EVIDENCE FOR SUPERSTELLAR METALLICITY*

THE LEECH EXOPLANET IMAGING SURVEY: ORBIT AND COMPONENT MASSES OF THE INTERMEDIATE-AGE, LATE-TYPE BINARY NO UMa* †

First light of the VLT planet finder SPHERE

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