WASP-128b: a transiting brown dwarf in the dynamical-tide regime

Kunovac, Vedad; Triaud, A. H. M. J.; Anderson, D. R.; Bouchy, F.; Cameron, A. Collier; Delrez, Laetitia; Gillon, M.; Hellier, C.; Jehin, Emmanuël; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Udry, S.; West, R. G.

doi:10.1093/mnras/sty2512

Cited by 36 publications

(20 citation statements)

References 56 publications

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“…The binary lightcurve software ellc was used to generate orbital and light curve models [22], and we employed the affineinvariant MCMC sampler emcee to explore parameter space [23]. We validated our approach [60,14] by re-analysing data from the eclipsing binary system WW Aurigae [61] and found a 1σ agreement with reported values.…”

Section: Global Analysis Of the Radial Velocity And Photometric Datamentioning

confidence: 80%

An eclipsing substellar binary in a young triple system discovered by SPECULOOS

et al. 2020

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corresponding authors Mass, radius, and age are three of the most fundamental parameters for celestial objects, enabling studies of the evolution and internal physics of stars, brown dwarfs, and planets. Brown dwarfs are hydrogen-rich objects that are unable to sustain core fusion reactions but are supported from collapse by electron degeneracy pressure [1]. As they age, brown dwarfs cool, reducing their radius and luminosity. Young exoplanets follow a similar behaviour. Brown dwarf evolutionary models are relied upon to infer the masses, radii and ages of these objects [2, 3]. Similar models are used to infer the mass and radius of directly imaged exoplanets [4]. Unfortunately, only sparse empirical mass, radius and age measurements are currently available, and the models remain mostly unvalidated. Double-line eclipsing binaries provide the most direct route for the absolute determination of the masses and radii of stars [5, 6, 7]. Here, we report the SPECULOOS discovery of 2M1510A, a nearby, eclipsing, double-line brown dwarf binary, with a widely-separated tertiary brown dwarf companion. We also find that the system is a member of the 45±5 Myr-old moving group, Argus [8, 9]. The system's age matches those of currently known directly-imaged exoplanets. 2M1510A provides an opportunity to benchmark evolutionary models of brown dwarfs and young planets. We find that widely-used evolutionary models [4] do reproduce the mass, radius and age of the binary components remarkably well, but overestimate the luminosity by up to 0.65 magnitudes, which could result in underestimated photometric masses for directly-imaged exoplanets and young field brown dwarfs by 20 to 35%.

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Section: Global Analysis Of the Radial Velocity And Photometric Datamentioning

confidence: 80%

An eclipsing substellar binary in a young triple system discovered by SPECULOOS

et al. 2020

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“…TOI-503b has an intermediate-mass of 53.7 ± 1.2 M J , an inclination angle of 82.25 +0.31 −0.41 degrees (b = 0.974 +0.022 −0.015 ), and lies in the driest part of the brown dwarf desert (35-55 M J sin i, P ≤ 100 days, Ma & Ge (2014b)). There is a paucity of objects detected in this driest region of the brown dwarf desert, but in recent years, 5 BDs (Gillen et al (2017), Nowak et al (2017), Hodžić et al (2018), Carmichael et al (2019), Persson et al (2019), and this work) have been discovered in this intermediate mass-range, bringing new life, so to speak, to the desert and increasing the overall tally in the aforementioned range to 6. The recent growth in the discoveries of this type of BDs could be a hint at an undisclosed population in the driest part of the BD desert.…”

Section: The Transiting Bd Populationmentioning

confidence: 58%

TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission*

Šubjak¹,

Sharma²,

Carmichael³

et al. 2020

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We report the discovery of an intermediate-mass transiting brown dwarf (BD), TOI-503b, from the TESS mission. TOI-503b is the first BD discovered by TESS, and it has circular orbit around a metallic-line A-type star with a period of P = 3.6772 ± 0.0001 days. The light curve from TESS indicates that TOI-503b transits its host star in a grazing manner, which limits the precision with which we measure the BD’s radius ( ). We obtained high-resolution spectroscopic observations with the FIES, Ondřejov, PARAS, Tautenburg, and TRES spectrographs, and measured the mass of TOI-503b to be M b = 53.7 ± 1.2 . The host star has a mass of M ⋆ = 1.80 ± 0.06 M ⊙, a radius of R ⋆ = 1.70 ± 0.05R ⊙, an effective temperature of T eff = 7650 ± 160 K, and a relatively high metallicity of 0.61 ± 0.07 dex. We used stellar isochrones to derive the age of the system to be ∼180 Myr, which places its age between that of RIK 72b (a ∼10 Myr old BD in the Upper Scorpius stellar association) and AD 3116b (a ∼600 Myr old BD in the Praesepe cluster). Given the difficulty in measuring the tidal interactions between BDs and their host stars, we cannot precisely say whether this BD formed in situ or has had its orbit circularized by its host star over the relatively short age of the system. Instead, we offer an examination of plausible values for the tidal quality factor for the star and BD. TOI-503b joins a growing number of known short-period, intermediate-mass BDs orbiting main-sequence stars, and is the second such BD known to transit an A star, after HATS-70b. With the growth in the population in this regime, the driest region in the BD desert ( ) is reforesting.

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“…Some binaries could be formed at the middle of the BDD, because of some scarce initial conditions. We need more similar systems, followed by in-depth studies, to understand the nature of these special cases (e.g., WASP-128b, Hodžić et al 2018).…”

Section: Discussionmentioning

confidence: 99%

“…cores (e.g., Kumar 1962Kumar , 1963Hayashi & Nakano 1963). In this view, the few detected brown-dwarf (BD) secondaries with short orbital periods (e.g., Bouchy et al 2011;Triaud et al 2017;Grieves et al 2017;dos Santos et al 2017;Beatty et al 2018;Hodžić et al 2018) are just oases found inside the 'desert'.…”

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confidence: 99%

Study of the Mass-Ratio Distribution of Spectroscopic Binaries. II. The Boundaries of the Brown-Dwarf Desert as Seen with the APOGEE Spectroscopic Binaries

Shahaf

Mazeh

2019

Monthly Notices of the Royal Astronomical Society

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Analysis of APOGEE DR12 stellar radial-velocities by Troup et al. (2016) affirmed the existence of the well-known Brown-Dwarf Desert (BDD). They detected a dearth of spectroscopic binaries (SB) with periods shorter than ∼ 10-30 days and secondaries with masses in the range of ∼ 0.01-0.1 M . We reconsider here their sample of binaries, focusing on 116 systems on the main sequence of the Gaia color-magnitude diagram, with mostly K-dwarf primaries. Using our recently devised algorithm to analyze the mass-ratio distribution of a sample of SBs we confirm the BDD existence and delineate its boundaries. For the K-dwarf APOGEE 1-25 days binaries, the companion-mass range of the BDD is ∼ 0.02-0.2 M . The mass ratio distribution of the long-period (25-500 days) binaries does not show any dearth at the q-range studied. Instead, their distribution displays a linear increase in log q, implying a tendency towards low-q values. The limits of the BDD do not coincide with the frequently used mass limits of the brown-dwarf population, sometimes defined as 0.013 and 0.08 M , based on theoretically derived stellar minimum masses for burning deuterium and hydrogen in their cores. Trying to draw the boundaries of the desert, we suggest either a wedged or trapezoidal shape. We discuss briefly different scenarios that can account for the formation of the BDD, in terms of differentiating between stellar secondaries and planets in particular, and compare this desert to the Neptunian desert that can distinguish between Jovian planets and super Earths of short periods.

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WASP-128b: a transiting brown dwarf in the dynamical-tide regime

Cited by 36 publications

References 56 publications

An eclipsing substellar binary in a young triple system discovered by SPECULOOS

An eclipsing substellar binary in a young triple system discovered by SPECULOOS

TOI-503: The First Known Brown-dwarf Am-star Binary from the TESS Mission*

Study of the Mass-Ratio Distribution of Spectroscopic Binaries. II. The Boundaries of the Brown-Dwarf Desert as Seen with the APOGEE Spectroscopic Binaries

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