Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Bowler, Brendan P.; Liu, Mengmeng; Shkolnik, Evgenya L.; Dupuy, Trent J.

doi:10.1088/0004-637x/774/1/55

Cited by 131 publications

(155 citation statements)

References 133 publications

(208 reference statements)

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“…For that purpose, we smoothed the low-resolution spectra of the objects to the resolution of the narrowest IRDIS filter, used the IRDIS filter pass-bands, a model of the Paranal atmospheric transmission generated with the ESO Skycalc web application 2 (Noll et al 2012;Jones et al 2013), and a model spectrum of Vega (Bohlin 2007). The same procedure was applied to the continuous 1.1−2.5 µm spectra of the moderately young companions HN Peg B (age ∼ 0.3 ± 0.2 Gyr, Luhman et al 2007), VHS 1256-1257 B (Gauza et al 2015), the younger companion 2MASS J01225093-2439505 b (possibly ∼10-120 Myr old, Bowler et al 2013;Rojo et al, in prep. ).…”

Section: Colorsmentioning

confidence: 99%

“…Most of them are found orbiting at large separations ( 50 AU) around young A&A 587, A58 (2016) and young nearby associations (Lucas et al 2001;Kirkpatrick et al 2006;Lodieu et al 2008;Rice et al 2010;Alves de Oliveira et al 2012Allers & Liu 2013;Gagné et al 2014a,b;Bonnefoy et al 2014a;Dawson et al 2014;Zapatero Osorio et al 2014). Among them, 2MASSW J1207334-393254 b (hereafter 2M1207b; Chauvin et al 2004), 2MASS J01225093-2439505 b (Bowler et al 2013), and VHS J125601.92-125723.9 b (Gauza et al 2015) appear to lie at the transition between the cloudy L-type and cloudless T-type dwarfs. Because they orbit stars with known distance, age, and (sometimes) metallicity, these rare young L/T-type companions offer the opportunity to study the key processes driving the disappearance of dust grains in the atmosphere of planets and brown dwarfs (e.g.…”

Section: Introductionmentioning

confidence: 99%

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First light of the VLT planet finder SPHERE

Bonnefoy¹,

Zurlo²,

Baudino³

et al. 2016

A&A

132

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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Section: Colorsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

First light of the VLT planet finder SPHERE

Bonnefoy¹,

Zurlo²,

Baudino³

et al. 2016

A&A

132

104

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“…These targets offer us one of the best opportunities to image exoplanets using high-contrast imaging. The dimmer host star in addition to a hotter planet (because of to its youth) significantly reduces contrast constraints (Chauvin et al 2015;Bowler et al 2013). Additionally, the young associations currently appear to be very incomplete for low-mass stars.…”

Section: Introductionmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2016

A&A

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Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. Aims. We search the field of view of 542 previously identified members of the young associations to identify wide or extremely wide (1000−100 000 au in physical separation) companions. Methods. We combined 2MASS near-infrared photometry (J, H, K) with proper motion values (from UCAC4, PPMXL, NOMAD) to identify companions in the field of view of known members. We collated further photometry and spectroscopy from the literature and conducted our own high-resolution spectroscopic observations for a subsample of candidate members. This complementary information allowed us to assess the efficiency of our method. Results. We identified 84 targets (45: 0.2−1.3 M , 17: 0.08−0.2 M , 22: <0.08 M ) in our analysis, ten of which have been identified from spectroscopic analysis in previous young association works. For 33 of these 84, we were able to further assess their membership using a variety of properties (X-ray emission, UV excess, H α , lithium and K I equivalent widths, radial velocities, and CaH indices). We derive a success rate of 76-88% for this technique based on the consistency of these properties. Conclusions. Once confirmed, the targets identified in this work would significantly improve our knowledge of the lower mass end of the young associations. Additionally, these targets would make an ideal new sample for the identification and study of planets around nearby young stars. Given the predicted substellar mass of the majority of these new candidate members and their proximity, high-contrast imaging techniques would facilitate the search for new low-mass planets.

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“…We see now the young field L and T dwarfs have a systematic offset relative to the field objects of ≈200-300 K cooler, while the young late-M dwarfs tend to run hotter than the field objects. A similar offset appears to be present between young companions and old field objects though less distinct (see also Bowler et al 2013), perhaps reflecting the more heterogeneous spectral typing of companion discoveries or (more speculatively) the possibility that young companion and young field objects behave differently. How do the T eff 's determined by fitting model atmospheres compare to the T eff 's determined from evolutionary models?…”

Section: Atmospheric and Evolutionary Modelsmentioning

confidence: 75%

“…Summary of T eff as a function of spectral type for ultracool dwarfs. Field (old) objects (grey) and young companions (blue) are from the calculations and compilation by Bowler et al(2013), with additions from Naud et al(2014) and Gauza et al(2015). Young field objects (orange) are primarily from Liu et al(in prep), with additional objects from , Gizis et al(2015), and Gagne et al(2015).…”

Section: Atmospheric and Evolutionary Modelsmentioning

confidence: 99%

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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Planets Around Low-Mass Stars. Iii. A Young Dusty L Dwarf Companion at the Deuterium-Burning Limit,

Cited by 131 publications

References 133 publications

First light of the VLT planet finder SPHERE

First light of the VLT planet finder SPHERE

Search for associations containing young stars (SACY)

What Do Young Brown Dwarfs Tell Us About Exoplanets?

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