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Prieur, Jean‐Louis; Koechlin, Laurent; Andre, C.; Gallou, G.; Lucuix, Christian

doi:10.1023/a:1008008110663

Cited by 31 publications

(38 citation statements)

References 18 publications

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“…Many such projects have been completed in the last few years (e.g., Mason et al 2004aMason et al , 2004bPrieur et al 2003;Scardia et al 2005). Substantial technical and programming improvements, as well as the widespread use of CCD cameras among small observatories and amateur astronomers, make it possible to perform both speckle observations of binary stars (with quite good precision) and diffraction-limited speckle imaging of compact extended objects.…”

Section: Introductionmentioning

confidence: 99%

Speckle Observations of Binary Stars with a 0.5 m Telescope

Rutkowski

Waniak

2005

PUBL ASTRON SOC PAC

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ABSTRACT. We present 36 observations of 17 visual binaries of moderate separation (ranging from 0Љ .15 to 0Љ .790) made with the 50 cm Cassegrain telescope of the Jagiellonian University in Kraków. The speckle interferometry technique was combined with modest optical hardware and a standard photometric CCD camera. We used broadband VRI filters without a Risley prism to reduce differential color refraction. Thus, we performed a model analysis to investigate the influence of this effect on the results of the measurements. For binary components of spectral type O-F, the difference of three spectral classes between them should bias their relative positions by no more than a couple of tens of milliarcseconds (mas) for moderate zenith distances. The statistical analysis of our results confirmed this conclusion. A cross-spectrum approach was applied to resolve the quadrant ambiguity. Our separations have rms deviations of 0Љ .012, and our position angles have rms deviations of 1Њ .8. Relative photometry in V, R, and I filters appeared to be the less accurately determined parameter. We discuss our errors in detail and compare them to other speckle data. This comparison clearly shows the quite good accuracy of our measurements. We also present an example of the enhancement of image resolution for an extended object with an angular size that is greater than the atmospheric coherence patch, using speckle interferometry techniques.

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Section: Introductionmentioning

confidence: 99%

Speckle Observations of Binary Stars with a 0.5 m Telescope

Rutkowski

Waniak

2005

PUBL ASTRON SOC PAC

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“…This instrumentation is presented in Prieur et al (1998) and our observing procedure is described in detail in Paper VI. For the present observations, thanks to an improvement of our software and a faster computer, we were also able to compute in real time the restricted triple correlation (Aristidi et al 1997) that we use for resolving the 180…”

Section: Observations and Description Of The Samplementioning

confidence: 99%

Speckle observations with PISCO in Merate: VIII. Astrometric measurements of visual binaries in 2007 and new orbits of the multiple system Zeta Aqr

et al. 2010

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We present relative astrometric measurements of visual binaries made during the second semester of 2007, with the speckle camera PISCO at the 102 cm Zeiss telescope of Brera Astronomical Observatory, in Merate. Our sample contains orbital couples as well as binaries whose motion is still uncertain. We obtained 283 new measurements of 279 objects, with angular separations in the range 0. 17-4. 4, and an average accuracy of 0. 014. The mean error on the position angles is 0.• 6. Most of the position angles were determined without the usual 180• ambiguity with the application of triplecorrelation techniques and/or by inspection of the long integration files. We also present the new orbit we have computed for Zeta Aqr AB (ADS 15971), for which our measurements lead to large residuals with the previously computed orbit. We were also able to compute the elements of the perturbation orbit Bb-P caused by an invisible companion, whose mass is estimated at 0.7 M .

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“…Details of the instrument can be found elsewhere (Prieur et al 1998). Particular care has been taken with the calibration of scale and orientation in the plane of the detector by the use of an objective grating (Scardia et al 2006a).…”

Section: The Orbitmentioning

confidence: 99%