Observations of binary stars by speckle interferometry – III

Morgan, B. L.; Beckmann, G. K.; Scaddan, R. J.; Vine, H. A.

doi:10.1093/mnras/198.3.817

Cited by 9 publications

(6 citation statements)

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“…In their infrared speckle program, Patience et al (1998) did not detect a speckle companion for γ Tau, but placed a limit to the K band magnitude difference of ∆K = 1.04 for the system. We did not detect a separated fringe packet for the star in any of our observations, and hence we suggest that the detection from Morgan et al (1982) may be spurious. The speckle binary, θ 1 Tau, is also a SB1 (Torres et al 1997, and references therein).…”

Section: Observations and Data Reductionmentioning

confidence: 49%

“…For instance, δ 1 Tau is a SB1 with a Mdwarf companion (Griffin & Gunn 1977) and ǫ Tau is an exo-planet host star (Sato et al 2007). γ Tau was resolved a single time as a speckle binary (with a large delta magnitude at 5000 Å) by Morgan et al (1982), having a system separation of 0.395 arcseconds. Since this measurement, it has remained undetected as a binary by other programs (McAlister 1978;Mason et al 1993;Patience et al 1998).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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Angular Diameters of the Hyades Giants Measured With the Chara Array

Boyajian

McAlister

Cantrell

et al. 2009

ApJ

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We present angular diameters of the Hyades giants, γ, δ 1 , ǫ, and θ 1 Tau from interferometric measurements with the CHARA Array. Our errors in the limb-darkened angular diameters for these stars are all less than 2%, and in combination with additional observable quantities, we determine the effective temperatures, linear radii and absolute luminosities for each of these stars. Additionally, stellar masses are inferred from model isochrones to determine the surface gravities. These data show that a new calibration of effective temperatures with errors well under 100K is now possible from interferometric angular diameters of stars.

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Section: Observations and Data Reductionmentioning

confidence: 49%

Section: Observations and Data Reductionmentioning

confidence: 99%

Angular Diameters of the Hyades Giants Measured With the Chara Array

Boyajian

McAlister

Cantrell

et al. 2009

ApJ

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“…Despite the duplicity of δ 1 Tau, its secular parallax solution is well defined (π sec,Hip = 21.16 ± 0.37 mas with g Hip = 0.07 and 21 Although γ Tau was reported as ρ ∼ 0. 395 speckle double by Morgan et al (1982), Mason et al (1993) and Patience et al (1998) could not confirm this result. Griffin & Holweger (1989) summarize the confusing literature on (non-existent) radial velocity variability, and conclude the object is single.…”

Section: B2 the Giants δ 1 And θ 1 Tau And δ Arimentioning

confidence: 84%

A Hipparcos study of the Hyades open cluster

Bruijne¹,

Hoogerwerf²,

Zeeuw³

2001

A&A

165

175

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Abstract. Hipparcos parallaxes fix distances to individual stars in the Hyades cluster with an accuracy of ∼6 percent. We use the Hipparcos proper motions, which have a larger relative precision than the trigonometric parallaxes, to derive ∼3 times more precise distance estimates, by assuming that all members share the same space motion. An investigation of the available kinematic data confirms that the Hyades velocity field does not contain significant structure in the form of rotation and/or shear, but is fully consistent with a common space motion plus a (one-dimensional) internal velocity dispersion of ∼0.30 km s −1 . The improved parallaxes as a set are statistically consistent with the Hipparcos parallaxes. The maximum expected systematic error in the proper motion-based parallaxes for stars in the outer regions of the cluster (i.e., beyond ∼2 tidal radii ∼20 pc) is < ∼ 0.30 mas. The new parallaxes confirm that the Hipparcos measurements are correlated on small angular scales, consistent with the limits specified in the Hipparcos Catalogue, though with significantly smaller "amplitudes" than claimed by Narayanan & Gould. We use the Tycho-2 long time-baseline astrometric catalogue to derive a set of independent proper motion-based parallaxes for the Hipparcos members. The new parallaxes provide a uniquely sharp view of the three-dimensional structure of the Hyades. The colour-absolute magnitude diagram of the cluster based on the new parallaxes shows a well-defined main sequence with two "gaps"/"turn-offs". These features provide the first direct observational support of Böhm-Vitense's prediction that (the onset of) surface convection in stars significantly affects their (B − V ) colours. We present and discuss the theoretical Hertzsprung-Russell diagram (log L versus log T eff ) for an objectively defined set of 88 high-fidelity members of the cluster as well as the δ Scuti star θ 2 Tau, the giants δ 1 , θ 1 , , and γ Tau, and the white dwarfs V471 Tau and HD 27483 (all of which are also members). The precision with which the new parallaxes place individual Hyades in the Hertzsprung-Russell diagram is limited by (systematic) uncertainties related to the transformations from observed colours and absolute magnitudes to effective temperatures and luminosities. The new parallaxes provide stringent constraints on the calibration of such transformations when combined with detailed theoretical stellar evolutionary modelling, tailored to the chemical composition and age of the Hyades, over the large stellar mass range of the cluster probed by Hipparcos.

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“…A number, including δ Vel were found to be double at separations of 10 mas and greater. Using the Anglo Australian Telescope and the Imperial College speckle interferometer (Morgan et al 1982) to try and resolve some of these stars, led to a paper by Tango et al (1979). The authors stated that the subsequent fringes found in the autocorrellograms of δ Vel which indicated a companion at a distance of about 0.…”

Section: Wds 05248-5219 I 345 Hip 25298mentioning

confidence: 99%