Astrometric and photometric measurements of binary stars with adaptive optics: observations from 2001 to 2006

Roberts, Lewis C.; Mason, Brian D.

doi:10.1093/mnras/stx2559

Cited by 18 publications

(20 citation statements)

References 60 publications

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“…CHR59=WDS17005+0635: This system is classified as Grade 4 on the USNO orbit catalogue. We find a large change in eccentricity from the previous orbit by Roberts & Mason (2018). This latter is based on adaptive optics observations from 2001 to 2006, and leads to e = 0.017 ± 0.021 in contrast to our value of 0.0814 ± 0.0070.…”

Section: Fin297ab=wds13145−2417contrasting

confidence: 78%

Orbits and masses of binaries from Speckle Interferometry at SOAR

Mendez,

Claveria,

Costa

2021

Preprint

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We present results from Speckle inteferometric observations of fifteen visual binaries and one doubleline spectroscopic binary, carried out with the HRCam Speckle camera of the SOAR 4.1 m telescope. These systems were observed as a part of an on-going survey to characterize the binary population in the solar vicinity, out to a distance of 250 parsec.We obtained orbital elements and mass sums for our sample of visual binaries. The orbits were computed using a Markov Chain Monte Carlo algorithm that delivers maximum likelihood estimates of the parameters, as well as posterior probability density functions that allow us to evaluate their uncertainty. Their periods cover a range from 5 yr to more than 500 yr; and their spectral types go from early A to mid M -implying total system masses from slightly more than 4 M down to 0.2 M . They are located at distances between approximately 12 and 200 pc, mostly at low Galactic latitude.For the double-line spectroscopic binary YSC8 we present the first combined astrometric /radial velocity orbit resulting from a self-consistent fit, leading to individual component masses of 0.897 ± 0.027 M and 0.857 ± 0.026 M ; and an orbital parallax of 26.61 ± 0.29 mas, which compares very well with the Gaia DR2 trigonometric parallax (26.55 ± 0.27 mas).In combination with published photometry and trigonometric parallaxes, we place our objects on an H-R diagram and discuss their evolutionary status. We also present a thorough analysis of the precision and consistency of the photometry available for them.

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Section: Fin297ab=wds13145−2417contrasting

confidence: 78%

Orbits and masses of binaries from Speckle Interferometry at SOAR

Mendez,

Claveria,

Costa

2021

Preprint

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“…Figure A1. Common proper motion analysis of τ Gem and its companion over the ∼10 year baseline between Gaia DR2 (red cross) and the astrometry from 2004 data provided by Roberts & Mason (2018) (red square). The black line shows the motion of a background object relative to τ Gem based on the Gaia DR2 parallax and proper motion of the primary, and the red dot indicates the expected position of a background object at the epoch of the 2MASS observations.…”

Section: Discussionmentioning

confidence: 99%

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

Fontanive

Rice

Bonavita

et al. 2019

Monthly Notices of the Royal Astronomical Society

119

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Stellar multiplicity is believed to influence planetary formation and evolution, although the precise nature and extent of this role remain ambiguous. We present a study aimed at testing the role of stellar multiplicity in the formation and/or evolution of the most massive, closein planetary and substellar companions. Using past and new direct imaging observations, as well as the Gaia DR2 catalogue, we searched for wide binary companions to 38 stars hosting massive giant planets or brown dwarfs (M > 7 M Jup ) on orbits shorter than ∼1 AU. We report the discovery of a new component in the WASP-14 system, and present an independent confirmation of a comoving companion to WASP-18. From a robust Bayesian statistical analysis, we derived a binary fraction of 79.0 +13.2 −14.7 % between 20−10,000 AU for our sample, twice as high as for field stars with a 3-σ significance. This binary frequency was found to be larger than for lower-mass planets on similar orbits, and we observed a marginally higher binary rate for inner companions with periods shorter than 10 days. These results demonstrate that stellar companions greatly influence the formation and/or evolution of these systems, suggesting that the role played by binary companions becomes more important for higher-mass planets, and that this trend may be enhanced for systems with tighter orbits. Our analysis also revealed a peak in binary separation at 250 AU, highlighting a shortfall of close binaries among our sample. This indicates that the mechanisms affecting planet and brown dwarf formation or evolution in binaries must operate from wide separations, although we found that the Kozai-Lidov mechanism is unlikely to be the dominant underlying process. We conclude that binarity plays a crucial role in the existence of very massive short-period giant planets and brown dwarf desert inhabitants, which are almost exclusively observed in multiple systems.

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“…(2018) orbit is indicated for comparison (dashed ellipse). The slightly increasing residuals at the end of the observations, that is at the end of the covered orbital arc, motivated the orbit solution of Roberts & Mason (2018). red pattern should reflect the mass ratio of Albireo Aa (K3 II) and Ac (B9 V).…”

Section: The Mass Of Albireo Aamentioning

confidence: 78%

“…Relative orbit of Albireo Ac (wrt Albireo Aa) according toRoberts & Mason (2018), including line of nodes (dash-dotted line), focal-point location (cross) and observations used for the orbit solution. Symbols and orientation are as inFig.…”

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confidence: 99%

The mass of Albireo Aa and the nature of Albireo AB

Bastian

Antón

2018

A&A

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Aims. We aim to clarify the nature of Albireo AB and specifically to decipher whether it is an optical or physical pair. We also try to determine the mass of Albireo Aa. Methods. We scrutinize and compare the available absolute astrometric data (from Hipparcos and Gaia DR2) of Albireo A and B, and we investigate the relative orbit of the pair Albireo Aa,Ac using orbit solutions based on ground-based interferometric measurements.Results. The mass of Albireo Aa (K3 II) is surprisingly small; only an upper limit of about 0.7 M could be derived. The systemic proper motion of Aa,Ac differs from that of component B by about 10 mas/year with an uncertainty of less than 2 mas/year. Albireo AB is therefore most probably an optical double. Conclusions. Specific astrometric and spectroscopic follow-up observations clarifying the surprising mass estimate for Albireo Aa are recommended.

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Astrometric and photometric measurements of binary stars with adaptive optics: observations from 2001 to 2006

Cited by 18 publications

References 60 publications

Orbits and masses of binaries from Speckle Interferometry at SOAR

Orbits and masses of binaries from Speckle Interferometry at SOAR

A high binary fraction for the most massive close-in giant planets and brown dwarf desert members

The mass of Albireo Aa and the nature of Albireo AB

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