Other
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19513805r&link_type=abstract
American Astronomical Society, 195th AAS Meeting, #138.05; Bulletin of the American Astronomical Society, Vol. 32, p.886
Other
Scientific paper
Traditionally speckle images are calibrated by observing a point source before or after the science observation. This point source observation is used to deconvolve the speckle transfer function (STF) from the energy spectrum of the science observation. Atmospheric seeing variations in time and over the sky ensure that the STF attenuation of the science object energy spectrum differs from that indicated by the calibration star STF. This difference leads to errors in the estimate of the object amplitude spectrum. To measure the quality of the calibration, V-band and R-band speckle observations of binary stars were taken with the 1.6-m telescope at the Air Force's Maui Space Surveillance Complex on Mt. Haleakala with the GEMINI speckle imaging system. Each binary star was observed five times, with a calibration star observed immediately after each observation. Half of the binaries used the same calibrator each time, while the other half used five different calibrators. The first set of observations was used to measure the precision of the processed image. The second set was used to measure the impact the separation between the science object and the calibrator has on the final image. The differential photometry of the binary was measured and used as an indicator of calibration quality.
Neyman Christopher R.
Roberts Lewis C. Jr.
Schulze Kathy J.
Stribling Bruce E.
Tyler David Wayne
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