Astron. J., 141, 180 (2011/June-0)
Observations of binary stars with the Differential Speckle Survey Instrument. III. Measures below the diffraction limit of the WIYN telescope.
HORCH E.P., VAN ALTENA W.F., HOWELL S.B., SHERRY W.H. and CIARDI D.R.
Abstract (from CDS):
In this paper, we study the ability of CCD- and electron-multiplying-CCD-based speckle imaging to obtain reliable astrometry and photometry of binary stars below the diffraction limit of the WIYN 3.5 m Telescope. We present a total of 120 measures of binary stars, 75 of which are below the diffraction limit. The measures are divided into two groups that have different measurement accuracy and precision. The first group is composed of standard speckle observations, that is, a sequence of speckle images taken in a single filter, while the second group consists of paired observations where the two observations are taken on the same observing run and in different filters. The more recent paired observations were taken simultaneously with the Differential Speckle Survey Instrument, which is a two-channel speckle imaging system. In comparing our results to the ephemeris positions of binaries with known orbits, we find that paired observations provide the opportunity to identify cases of systematic error in separation below the diffraction limit and after removing these from consideration, we obtain a linear measurement uncertainty of 3-4 mas. However, if observations are unpaired or if two observations taken in the same filter are paired, it becomes harder to identify cases of systematic error, presumably because the largest source of this error is residual atmospheric dispersion, which is color dependent. When observations are unpaired, we find that it is unwise to report separations below approximately 20 mas, as these are most susceptible to this effect. Using the final results obtained, we are able to update two older orbits in the literature and present preliminary orbits for three systems that were discovered by Hipparcos.
binaries: visual - techniques: high angular resolution - techniques: interferometric - techniques: photometric
In table 1 ** HDS 284 is a misprint for ** HDS 285. In table 2: WDS 19380+3354 is a misprint for WDS 19380+3353.
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