Discovery of a Wide Companion near the Deuterium-burning Mass Limit in the Upper Scorpius Association

Béjar, V. J. S.; Osorio, M. R. Zapatero; Pérez‐Garrido, A.; Álvarez, Carlos; Martín, E. L.; Rebolo, R.; Villó-Pérez, Isidro; Díaz‐Sánchez, A.

doi:10.1086/527557

Cited by 112 publications

(94 citation statements)

References 41 publications

(68 reference statements)

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“…comm.). Other similar systems, some of them with wider projected physical separations but without common proper-motion confirmation, have also been discovered in the Orion OB1 association (Caballero et al 2006;Barrado y Navascués et al 2007), Upper Scorpius (Kraus & Hillenbrand 2007;Béjar et al 2008), and highly extinguished star-forming regions in the Southern Hemisphere, such as Chamaeleon and Lupus (López Martí et al 2004Luhman 2004). …”

Section: A Comparison Of Binding Energiesmentioning

confidence: 92%

Reaching the boundary between stellar kinematic groups and very wide binaries

Caballero¹

2009

A&A

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Aims. I look for and characterise very wide binaries and multiple systems with projected physical separations larger than s = 0.1 pc, which is generally believed to be a sharp upper limit to the distribution of wide binary semimajor axes. Methods. I investigated in detail 30 Washington double stars with angular separations of ρ > 1000 arcsec. I discarded 23 of them as probably unbound systems based on discordant astrometry, photometry, spectral types, and radial velocities. The remaining seven systems were subject to a comprehensive data compilation and derivation (multi-wavelength photometry, heliocentric distance, multiplicity, age, mass, metallicity, membership in a young kinematic group). Results. Of the seven very wide systems, six have projected physical separations greater than the hypothetical cutoff at s = 0.1 pc and four have separations s > 0.2 pc. Although there are two systems in young kinematic groups (namely HD 136654 and BD+32 2572 in the Hyades Supercluster, and AU Mic and AT Mic AB in the β Pictoris moving group), there is no clear prevalence of young systems (τ < 1 Ga) among these very wide binaries. Finally, I compare the binding energies of the seven systems with those of other weakly bound systems in the field.

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Section: A Comparison Of Binding Energiesmentioning

confidence: 92%

Reaching the boundary between stellar kinematic groups and very wide binaries

Caballero¹

2009

A&A

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“…This resolution is sufficient to study atomic and molecular lines. The age-sequence is composed of spectra of members of the Taurus (KPNO Tau 4; Briceño et al 2002), Chameleon I (OTS 44; Oasa et al 1999;Luhman et al 2004), and Upper Scorpius (UScoCTIO 108B; Béjar et al 2008) star forming regions. We also overlay the spectrum of the M10III Mira IO Virginis (Rayner et al 2009) as an example of an extremely low surface gravity atmospheres.…”

Section: An Age-sequence Of M95 Dwarfsmentioning

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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“…Actually, with a mass close to the frontier between stars and brown dwarfs, vB 10 is the least-massive star with a known planet. Planets with wider orbits have been found by direct imaging techniques around young brown dwarfs (Chauvin et al 2004;Béjar et al 2008). vB 10 is also one of the closest low-mass systems (d = 5.9 pc) to the Sun.…”

Section: Introductionmentioning

confidence: 99%

Infrared radial velocities of vB 10

Osorio

Martín

Burgo

et al. 2009

A&A

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We present radial velocities of the M8V-type, very low-mass star vB 10 obtained at four different epochs between 2001 and 2008. We use high-resolution (R ∼ 20 000) near-infrared (J-band) spectra taken with the nirspec instrument on the Keck II telescope. Our data suggest that vB 10 shows radial velocity variability with an amplitude of ∼1 km s −1 , a result that is consistent with the recent finding of a massive planet companion around the star. More velocity measurements and a better sampling of the orbital phase are required to precisely constrain the orbital parameters and the individual masses of the pair.

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Discovery of a Wide Companion near the Deuterium-burning Mass Limit in the Upper Scorpius Association

Cited by 112 publications

References 41 publications

Reaching the boundary between stellar kinematic groups and very wide binaries

Reaching the boundary between stellar kinematic groups and very wide binaries

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

Infrared radial velocities of vB 10

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