Other
Scientific paper
Sep 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...19411202r&link_type=abstract
American Astronomical Society Meeting 194, #112.02
Other
Scientific paper
The traditional way of calibrating a speckle image is to observe a point source before or after the science observation. This point source observation is then used to deconvolve the speckle transfer function (STF) from the energy spectrum of the science observation. 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 will lead to errors in the estimate of the object amplitude spectrum. To measure the effects of this miscalibration, V-band and R-band speckle observations of binary stars were taken at the 1.6-m telescope at the Air Force's Maui Space Surveillance Complex on Haleakala with the GEMINI 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 images and 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 the binary was measured and used as a indicator of miscalibration.
Neyman Christopher R.
Roberts Lewis C. Jr.
Schulze Kathy J.
Stribling Bruce E.
Tyler David Wayne
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