The Orbit of the Brown Dwarf Binary Gliese 569B

Lane, Benjamin F.; Osorio, M. R. Zapatero; Britton, M. C.; Martín, E. L.; Kulkarni, S. R.

doi:10.1086/322506

Cited by 95 publications

(122 citation statements)

References 49 publications

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“…We are searching for sub-stellar companions also on the southern sky, with speckle and normal imaging at the ESO NTT, and now also with AO (NAOS-CONICA at the ESO VLT). Four sub-stellar companions to young (nearby) stars have been confirmed by both proper motion and spectroscopy: The ∼12 Myrs young TWA-5 B (Lowrance et al 1999;Neuhäuser et al 2000), the ∼300 Myrs old Gl 569 B, C Lane et al 2001), the ∼35 Myrs young HR 7239 B (Lowrance et al 2000;Guenther et al 2001), and the ∼300 Myrs old HD 130948 B, C (Potter et al 2002;Goto et al 2002).…”

Section: Introductionmentioning

confidence: 86%

HD 77407 and GJ 577: Two new young stellar binaries

Mugrauer

Neuhäuser

Guenther

et al. 2004

A&A

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Abstract. We present the first results from our search for close stellar and sub-stellar companions to young nearby stars on the northern sky. Our infrared imaging observations are obtained with the 3.5 m Calar Alto telescope and the AO system ALFA. With two epoch observations which were separated by about one year, we found two co-moving companion candidates, one close to HD 77407 and one close to GJ 577. For the companion candidate near GJ 577, we obtained an optical spectrum showing spectral type M 4.5; this candidate is a bound low-mass stellar companion confirmed by both proper motion and spectroscopy. We estimate the masses for HD 77407 B and GJ 577 B to be ∼0.3 to 0.5 M and ∼0.16 to 0.2 M , respectively. Compared to Siess et al. (2000) models, each of the two pairs appears co-eval with HD 77407 A, B being 10 to 40 Myrs and GJ 577 A, B being ≥100 Myrs old. We also took multi-epoch high-resolution spectra of HD 77407 to search for sub-stellar companions, but did not find any with 3 M Jup as upper mass (m sin i) limit (for up to 4 year orbits); however, we detected a long-term radial velocity trend in HD 77407 A, consistent with a ∼0.3 M companion at ∼50 AU separation, i.e. the one detected by the imaging. Hence, HD 77407 B is confirmed to be a bound companion to HD 77407 A. We also present limits for undetected, but detectable companions using a deep image of HD 77407 A and B, also observed with the Keck NIRC2 AO system; any brown dwarfs were detectable outside of 0.5 arcsec (17 AU at HD 77407), giant planets with masses from ∼6.5 to 12 M Jup were detectable at ≥1.5 arcsec.

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Section: Introductionmentioning

confidence: 86%

HD 77407 and GJ 577: Two new young stellar binaries

Mugrauer

Neuhäuser

Guenther

et al. 2004

A&A

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“…Lane et al 2001;Bouy et al 2003;Siegler et al 2005;Forveille et al 2005;Burgasser & McElwain 2006;Caballero 2007a -see also Bouy et al 2005 andBurgasser et al 2007 for compilations); -"classic" systems in the Solar neighbourhood with late-Mtype companions and q < 0.5, such us V1054 Oph + GJ 643 + vB 8, GX And + GQ And, EQ Peg AB, V1428 Aql + vB 10, and o 2 Eri AC; -field stellar systems with late-M-, L-, and T-type companions and q < 0.5 (e.g. Rebolo et al 1998;Goldman et al 1999;Burgasser et al 2000;Kirkpatrick et al 2001;Gizis et al 2001;Scholz et al 2003;Seifahrt et al 2005).…”

Section: A Comparison Of Binding Energiesmentioning

confidence: 99%

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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“…Properties of the host star are more readily measured and may be used to infer those of the companion, such as chemical composition or possibly age, under the assumption that the star and brown dwarf formed from the same material at the same time (Pinfield et al 2006). A number of these "benchmark" systems have recently been discovered (Lane et al 2001;Close et al 2005;Liu et al 2007;Ireland et al 2008;Dupuy et al 2009a;Bowler et al 2009;Biller et al 2010;Wahhaj et al 2011).…”

Section: Introductionmentioning

confidence: 99%

The Dynamical Mass and Three-Dimensional Orbit of Hr7672b: A Benchmark Brown Dwarf With High Eccentricity

Crepp

Johnson

Fischer

et al. 2012

ApJ

103

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The companion to the G0V star HR7672 directly imaged by Liu et al. has moved measurably along its orbit since the discovery epoch, making it possible to determine its dynamical properties. Originally targeted with adaptive optics because it showed a long-term radial velocity (RV) acceleration (trend), we have monitored this star with precise Doppler measurements and have now established a 24 year time baseline. The RV variations show significant curvature (change in the acceleration) including an inflection point. We have also obtained a recent image of HR7672B with NIRC2 at Keck. The astrometry also shows curvature. In this paper, we use jointly fitted Doppler and astrometric models to calculate the three-dimensional orbit and dynamical mass of the companion. The mass of the host star is determined using a direct radius measurement from CHARA interferometry in combination with high-resolution spectroscopic modeling. We find that HR7672B has a highly eccentric, e = 0.50 +0.01 −0.01 , near edge-on, i = 97.3 +0.4 −0.5 deg, orbit with semimajor axis, a = 18.3 +0.4 −0.5 AU. The mass of the companion is m = 68.7 +2.4 −3.1 M J . HR7672B thus resides near the substellar boundary, just below the hydrogen-fusing limit. These measurements of the companion mass are independent of its brightness and spectrum and establish HR7672B as a rare and precious "benchmark" brown dwarf with a well-determined mass, age, and metallicity essential for testing theoretical evolutionary models and synthetic spectral models. Indeed, we find that such models under-predict its luminosity by a factor of ≈2. HR 7672B is presently the only L, T, or Y dwarf known to produce an RV trend around a solar-type star.

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The Orbit of the Brown Dwarf Binary Gliese 569B

Cited by 95 publications

References 49 publications

HD 77407 and GJ 577: Two new young stellar binaries

HD 77407 and GJ 577: Two new young stellar binaries

Reaching the boundary between stellar kinematic groups and very wide binaries

The Dynamical Mass and Three-Dimensional Orbit of Hr7672b: A Benchmark Brown Dwarf With High Eccentricity

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