Thermal Infrared Mmtao Observations of the Hr 8799 Planetary System

Hinz, Philip M.; Rodigas, Timothy J.; Kenworthy, Matthew A.; Sivanandam, Suresh; Heinze, A.; Mamajek, Eric E.; Meyer, Michael

doi:10.1088/0004-637x/716/1/417

Cited by 121 publications

(169 citation statements)

References 73 publications

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“…HR 8799 (L = 5.220 ± 0.018, Hinz et al 2010) was observed on October 21 UT with the "DX" side of the telescope at two Notes. The seeing is the value measured by the LBT differential image motion monitor (DIMM) in the same direction on the sky as the target.…”

Section: Observations and Data Reductionmentioning

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

A&A

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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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Section: Observations and Data Reductionmentioning

confidence: 99%

Section: Orbital Architecturementioning

confidence: 99%

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

Maire

Skemer

Hinz

et al. 2015

A&A

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“…So far, studies of the atmospheres of HR8799 bcde were conducted using mostly photometric measurements in the infrared (1−5 µm; Marois et al 2008Marois et al , 2010Lafrenière et al 2009;Hinz et al 2010;Janson et al 2010;Currie et al 2011a;Galicher et al 2011;Skemer et al 2012;Esposito et al 2013;Skemer et al 2014;Currie et al 2014). The measurements indicate that the four planets add to the restrained list of young companions at the L/T transition.…”

Section: Introductionmentioning

confidence: 99%

“…Models with local variation of the cloud thickness ("patchy" clouds) have been proposed to improve the fit of the planet spectral energy distributions (SEDs; Currie et al 2011aCurrie et al , 2014Skemer et al 2012). At longer wavelengths, the planets show evidence for disequilibrium carbon chemistry, exhibiting weak CH 4 absorption at 3.3 µm and strong CO absorption at 5 µm (Hinz et al 2010;Janson et al 2010;Galicher et al 2011;Skemer et al 2012Skemer et al , 2014Currie et al 2014).…”

Section: Introductionmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Bonnefoy¹,

Zurlo²,

Baudino³

et al. 2016

A&A

127

104

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Context. The system of four planets discovered around the intermediate-mass star HR8799 offers a unique opportunity to test planet formation theories at large orbital radii and to probe the physics and chemistry at play in the atmospheres of self-luminous young (∼30 Myr) planets. We recently obtained new photometry of the four planets and low-resolution (R ∼ 30) spectra of HR8799 d and e with the SPHERE instrument (Paper III). Aims. In this paper (Paper IV), we aim to use these spectra and available photometry to determine how they compare to known objects, what the planet physical properties are, and how their atmospheres work. Methods. We compare the available spectra, photometry, and spectral energy distribution (SED) of the planets to field dwarfs and young companions. In addition, we use the extinction from corundum, silicate (enstatite and forsterite), or iron grains likely to form in the atmosphere of the planets to try to better understand empirically the peculiarity of their spectrophotometric properties. To conclude, we use three sets of atmospheric models (BT-SETTL14, Cloud-AE60, Exo-REM) to determine which ingredients are critically needed in the models to represent the SED of the objects, and to constrain their atmospheric parameters (T eff , log g, M/H). Results. We find that HR8799d and e properties are well reproduced by those of L6-L8 dusty dwarfs discovered in the field, among which some are candidate members of young nearby associations. No known object reproduces well the properties of planets b and c. Nevertheless, we find that the spectra and WISE photometry of peculiar and/or young early-T dwarfs reddened by submicron grains made of corundum, iron, enstatite, or forsterite successfully reproduce the SED of these planets. Our analysis confirms that only the Exo-REM models with thick clouds fit (within 2σ) the whole set of spectrophotometric datapoints available for HR8799 d and e for T eff = 1200 K, log g in the range 3.0−4.5, and M/H = +0.5. The models still fail to reproduce the SED of HR8799c and b. The determination of the metallicity, log g, and cloud thickness are degenerate. Conclusions. Our empirical analysis and atmospheric modelling show that an enhanced content in dust and decreased CIA of H 2 is certainly responsible for the deviation of the properties of the planet with respect to field dwarfs. The analysis suggests in addition that HR8799c and b have later spectral types than the two other planets, and therefore could both have lower masses.

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“…Its age has been estimated to be 20-160 Myr (Cowley et al 1969;Moór et al 2006;Marois et al 2008;Hinz et al 2010;Zuckerman et al 2011;Baines et al 2012), and the distance of the system is 39.4 ± 1.0 pc (van Leeuwen 2007). This system is a benchmark for the study of young, gaseous giant planets, their formation and evolution.…”

Section: Introductionmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Zurlo

Vigan

Galicher

et al. 2016

A&A

141

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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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Thermal Infrared Mmtao Observations of the Hr 8799 Planetary System

Cited by 121 publications

References 73 publications

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

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

First light of the VLT planet finder SPHERE

First light of the VLT planet finder SPHERE

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