Direct-imaging discovery of a 12–14 Jupiter-mass object orbiting a young binary system of very low-mass stars

Delorme, P.; Gagné, Jonathan; Girard, J.; Lagrange, A. M.; Chauvin, G.; Naud, Marie-Ève; Lafrenière, David; Doyon, René; Riedel, Adric R.; Bonnefoy, M.; Malo, Lison

doi:10.1051/0004-6361/201321169

Cited by 119 publications

(125 citation statements)

References 43 publications

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“…Delorme et al (2013) reported the discovery of a 12−14 M Jup orbiting a pair of young (30 Myr) late M-dwarfs (2M01033563-5515561) at a projected separation of 84 AU (system at 42 pc). Later on, Rameau et al (2013b) detected a probable 4 − 5 M Jup companion to the young (10 − 17 Myr) A star HD 95086 at a projected separation of 56 AU.…”

Section: Occurrence Of Giant Planets As a Function Of The Stellar Massmentioning

confidence: 99%

Giant planets around AF and M stars

Rameau¹,

Chauvin²,

Lagrange³

et al. 2013

Proc. IAU

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Abstract. We present the results of two three-year surveys of young and nearby stars to search for wide orbit giant planets. On the one hand, we focus on early-type and massive, namely β Pictoris analogs. On the other hand, we observe late type and very low mass stars, i.e., M dwarfs. We report individual detections of new planetary mass objects. According to our deep detection performances, we derive the observed frequency of giant planets between these two classes of parent stars. We find frequency between 6 to 12 % but we are not able to assess a/no correlation with the host-mass.

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Section: Occurrence Of Giant Planets As a Function Of The Stellar Massmentioning

confidence: 99%

Giant planets around AF and M stars

Rameau¹,

Chauvin²,

Lagrange³

et al. 2013

Proc. IAU

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“…Advances in high-contrast and high-resolution imaging in the NIR (1-5 µm) led to the discovery of late-type companions to young nearby stars straddling the planet/BD boundary (e.g., Chauvin et al 2004Chauvin et al , 2005Lafrenière et al 2008;Marois et al 2008Marois et al , 2010Lagrange et al 2010;Ireland et al 2011;Delorme et al 2013;Rameau et al 2013;Kuzuhara et al 2013;Currie et al 2014). Most of these objects have estimated effective temperatures similar to those of L dwarfs.…”

Section: Introductionmentioning

confidence: 99%

New constraints on the formation and settling of dust in the atmospheres of young M and L dwarfs

Manjavacas

Bonnefoy

Schlieder

et al. 2014

A&A

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Context. Gravity modifies the spectral features of young brown dwarfs (BDs). A proper characterization of these objects is crucial for the identification of the least massive and latest-type objects in star-forming regions, and to explain the origin(s) of the peculiar spectrophotometric properties of young directly imaged extrasolar planets and BD companions. Aims. We obtained medium-resolution (R ∼ 1500−1700) near-infrared (1.1−2.5 µm) spectra of seven young M9.5-L3 dwarfs classified at optical wavelengths. We aim to empirically confirm the low surface gravity of the objects in the near-infrared. We also test whether self-consistent atmospheric models correctly represent the formation and the settling of dust clouds in the atmosphere of young late-M and L dwarfs. Methods. We used the Infrared Spectrometer And Array Camera (ISAAC) at the Very Large Telescope (VLT) to obtain the spectra of the targets. We compared the spectra to those of mature and young BDs, and to young late-type companions to nearby stars with known ages to identify and study gravity-sensitive features. We computed spectral indices weakly sensitive to the surface gravity to derive near-infrared spectral types. Finally, we found the best fit between each spectrum and synthetic spectra from the BT-Settl 2010 and 2013 atmospheric models. Using the best fit, we derived the atmospheric parameters of the objects and identified which spectral characteristics the models do not reproduce. Results. We confirmed that our objects are young BDs and we found near-infrared spectral types in agreement with the ones determined at optical wavelengths. The spectrum of the L2γ dwarf 2MASSJ232252.99-615127.5 reproduces the spectrum of the planetary mass companion 1RXS J160929.1-210524b well. The BT-Settl models fit the spectra and the 1−5 µm spectral energy distribution of the L0-L3 dwarfs for temperatures between 1600−2000 K. But the models fail to reproduce the shape of the H band and the near-infrared slope of some of our targets. This fact, and the best-fit solutions found with super-solar metallicity, are indicative of a lack of dust, in particular at high altitude, in the cloud models. Conclusions. The modeling of the vertical mixing and of the grain growth will be revised in the next version of the BT-Settl models. These revisions may suppress the remaining non-reproducibilities. Our spectra provide additional templates for the characterization of the numerous young L-type companions that will be detected in the coming years by planet imaging instruments such as VLT/SPHERE, Gemini/GPI, Subaru/SCexAO, and LBTI/LMIRCam.

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“…We excluded from the list the massive planets or brown dwarfs in a wide orbit (a p > 80 a.u.) that were discovered by direct imaging (Ros 458 b, SR 12 c, 2MASS0103, FW Tau b and ROXs 42B b; Burgasser et al 2010;Kuzuhara et al 2011;Delorme et al 2013;Kraus et al 2014), because the large separation from the central stars makes the effects discussed here absolutely negligible. We also excluded binary systems with cataclysmic variables or white dwarfs (PSR B1620-26, HU Aqr, HW Vir, NN Ser, DP Leo, UZ For, RR Cae, and NY Vir; Sigurdsson et al 2003;Hinse et al 2012;Beuermann et al 2010Beuermann et al , 2011Beuermann et al , 2012Potter et al 2011;Qian et al 2012a,b), because the common-envelope evolution of the central system would cause a different astrophysical situation.…”

Section: Application To Current Circumbinary Planetsmentioning

confidence: 84%

Effects of X-ray and extreme UV radiation on circumbinary planets

Sanz-Forcada

Desidera

Micela

2014

A&A

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Context. Several circumbinary planets have recently been discovered. The orbit of a planet around a binary stellar system poses several dynamic constraints. In addition to these constraints, the effects that radiation from the host stars may have on the planet atmospheres must be considered. We here evaluate these effects. Because of the configuration of a close binary system, these stars have a high rotation rate, even for old stars. The fast rotation of close, tidally locked binaries causes a permanent state of high stellar activity and copious XUV radiation. The accumulated effects are stronger than for normal exoplanets around single stars and cause a faster evaporation of their atmospheres. Aims. We evaluate the effects that stellar radiation has on the evaporation of exoplanets around binary systems and on the survival of these planets. Methods. We considered the X-ray and EUV spectral ranges (XUV, 1-912 Å) to account for the photons that are easily absorbed by a planet atmosphere that is mainly composed of hydrogen. A more complex atmospheric composition is expected to absorb this radiation more efficiently. We used direct X-ray observations to evaluate the energy in the X-rays range and coronal models to calculate the (nondetectable) EUV part of the spectrum. Results. We considered in this problem different configurations of stellar masses, and a resonance of 4:1 and 3:1. The simulations show that exoplanets orbiting close binary systems in a close orbit will suffer strong photoevaporation that may cause a total loss of atmosphere in a short time. We also applied our models to the best real example, Kepler-47 b, to estimate the current mass-loss rates in circumbinary planets and the accumulated effects over the time. Conclusions. A binary system of two solar-like stars will be highly efficient in evaporating the atmosphere of the planet (less than 6 Gyr in our case). These systems will be difficult to find, even if they are dynamically stable. Still, planets may orbit around binary systems of low mass stars for wider orbits. Currently known circumbinary planets are not substantially affected by thermal photoevaporation processes, unless Kepler-47 b has an inflated atmosphere. The distribution of the orbital periods of circumbinary planets is shifted to much longer periods than the average of Kepler planets, which supports a scenario of strong photoevaporation in close-in circumbinary planets.

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Direct-imaging discovery of a 12–14 Jupiter-mass object orbiting a young binary system of very low-mass stars

Cited by 119 publications

References 43 publications

Giant planets around AF and M stars

Giant planets around AF and M stars

New constraints on the formation and settling of dust in the atmospheres of young M and L dwarfs

Effects of X-ray and extreme UV radiation on circumbinary planets

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