Reconnaissance of the Hr 8799 Exosolar System. I. Near-Infrared Spectroscopy

Oppenheimer, Ben R.; Baranec, Christoph; Beichman, Charles; Brenner, Douglas; Burruss, Rick; Cady, Eric; Crepp, Justin R.; Dekany, Richard; Fergus, Rob; Hale, David; Hillenbrand, Lynne A.; Hinkley, Sasha; Hogg, David W.; King, David L.; Ligon, E. R.; Lockhart, Thomas; Nilsson, Ricky; Parry, Ian; Pueyo, Laurent; Rice, Emily L.; Roberts, J. T.; Roberts, Lewis C.; Shao, Michael; Sivaramakrishnan, Anand; Soummer, Rémi; Truong, Trieu‐Kien; Vasisht, Gautam; Veicht, A.; Vescelus, F.; Wallace, J. Kent; Zhai, Chengxing; Zimmerman, Neil

doi:10.1088/0004-637x/768/1/24

Cited by 153 publications

(194 citation statements)

References 90 publications

(209 reference statements)

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“…Despite having incredible similarity in color and magnitude, these two objects have quite different spectral shapes. Overall, observations of young brown dwarfs and directly-imaged exoplanets (Gauza et al 2015) and HR 8799b (Barman et al 2011Oppenheimer et al 2013). The J − H color and absolute J -band magnitude of VHS 1256−1257B agree (to within the uncertainties) with photometry of the exoplanet, HR 8799b.…”

Section: Introductionsupporting

confidence: 55%

What Do Young Brown Dwarfs Tell Us About Exoplanets?

2015

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Abstract. In recent years, all-sky surveys have uncovered a new and interesting population of young (≈10-200 Myr), nearby substellar objects. Many of these objects have inferred masses and temperatures that overlap those of directly imaged exoplanets. These young brown dwarfs provide valuable analogs to young, dusty exoplanets in a context where detailed spectroscopic observations across a broad range of wavelengths and at high S/N are possible. How do the temperatures inferred by atmospheric models and evolutionary models compare? Can we determine the formation mechanism of a young planetary-mass object? How well do we understand the role that disequilibrium chemistry and dust clouds play in the atmospheres of these objects? We review the successes and challenges in determining the fundamental properties (mass, log(g), effective temperature) of young substellar objects, both brown dwarfs and gas-giant exoplanets.

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Section: Introductionsupporting

confidence: 55%

What Do Young Brown Dwarfs Tell Us About Exoplanets?

2015

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“…For fainter objects, such as the planets around the star HR 8799 (Marois et al 2008b), SPHERE would be able to detect HR 8799d, 7 M Jup planet at a distance of 27 AU (Marois et al 2010;Oppenheimer et al 2013), with a relative astrometric error of 3 mas. Esposito et al (2013), using LBT/PISCES, found an astrometric error of 10 mas.…”

Section: Discussionmentioning

confidence: 99%

“…On this datacube we used both the spectral deconvolution (SD, see e.g, Sparks & Ford 2002;Thatte et al 2007) and the principal component analysis (PCA, see, e.g, Amara & Quanz 2012;Soummer et al 2012;Oppenheimer et al 2013) reductions A85, page 4 of 13 methods. For more details, regarding the first method applied on SPHERE-IFS data we refer the reader to Mesa et al (2014).…”

Section: Data Reduction and Detection Limitsmentioning

confidence: 99%

“…A new generation of high-contrast imaging instruments specifically designed for direct imaging of extrasolar planets is now operational, such as the Project 1640 at the 5 m Palomar Telescope (Crepp et al 2011) which provides important science results (see, e.g, Oppenheimer et al 2013), or the Gemini Planet Finder (GPI, Macintosh et al 2014) at the Gemini South Telescope that just concluded its commissioning phase and already provides scientific results (Galicher et al 2014). A fourth instrument, the Coronagraphic High Angular Resolution Imaging Spectrograph (CHARIS, Peters-Limbach et al 2013), is expected to be operative at the Subaru Telescope at the end of 2015.…”

Section: Introductionmentioning

confidence: 99%

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Performance of the VLT Planet Finder SPHERE

Zurlo

Vigan

Mesa

et al. 2014

A&A

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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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“…Oppenheimer et al 2013;Allers & Liu 2013). This produces large scatter in the colours, with low-gravity objects -such as the late-L-type planet 2M1207b (Chauvin et al 2004) -usually having redder J−K colours.…”

Section: Discussionmentioning

confidence: 99%

CFBDS J111807-064016: A new L/T transition brown dwarf in a binary system

Reylé¹,

Delorme²,

Artigau³

et al. 2014

A&A

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Binary systems with a substellar companion are quite rare and provide interesting benchmarks. They constrain the complex physics of substellar atmospheres, because several physical parameters of the substellar secondary can be fixed from the much better characterized main-sequence primary. We report the discovery of CFBDS J111807-064016, a T2 brown-dwarf companion to 2MASS J111806.99-064007.8, a low-mass M4.5-M5 star. The brown dwarf was identified from the Canada France Brown Dwarf Survey. At a distance of 50-120 pc, the 7.7 angular separation corresponds to projected separations of 390-900 AU. The primary displays no H α emission, placing a lower limit on the age of the system of about 6 Gyr. The kinematics is also consistent with membership in the old thin disc. We obtained near-infrared spectra, which together with recent atmosphere models allow us to determine the effective temperature and gravity of the two components. We derived a system metallicity of [Fe/H] = −0.1 ± 0.1 using metallicity-sensitive absorption features in our medium-resolution K s spectrum of the primary. From these parameters and the age constraint, evolutionary models estimate masses of 0.10 to 0.15 M for the M dwarf and 0.06 to 0.07 M for the T dwarf. This system is a particularly valuable benchmark because the brown dwarf belongs to the early-T class: the cloud-clearing that occurs at the L/T transition is very sensitive to gravity, metallicity, and detailed dust properties, and produces a large scatter in the colours. This T2 dwarf, with its metallicity measured from the primary and its mass and gravity much better constrained than those of younger early-Ts, will anchor our understanding of the colours of L/T transition brown dwarfs. It is also one of the most massive T dwarfs, just below the hydrogen-burning limit, and all this makes it a prime probe for brown-dwarf atmosphere and evolution models.

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Reconnaissance of the Hr 8799 Exosolar System. I. Near-Infrared Spectroscopy

Cited by 153 publications

References 90 publications

What Do Young Brown Dwarfs Tell Us About Exoplanets?

What Do Young Brown Dwarfs Tell Us About Exoplanets?

Performance of the VLT Planet Finder SPHERE

CFBDS J111807-064016: A new L/T transition brown dwarf in a binary system

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