KEYWORDS: Charge-coupled devices, Signal detection, Back illuminated sensors, Photometry, Point spread functions, Stars, Signal to noise ratio, Linear filtering, Interference (communication), Staring arrays
A measurement program designed to investigate the variations in sensitivity of focal plane array son a sub-pixel scale has produced such information for two devices: a two-phase front-illuminated CCD and a three-phase back-illuminated CCD. The effect of a non-uniform pixel response on a aperture photometry has been previously analyzed for a front-illuminated CCD. This paper presents results regarding the photometric errors to be expected for a back-illuminated CCD and astrometric errors for both devices. The uncertainty introduced in both measurements, when using under sampled data, is significant.
KEYWORDS: Charge-coupled devices, Linear filtering, Signal detection, Point spread functions, Stars, Light sources, Optical filters, Back illuminated sensors, Diffusion, Sensors
This paper presents results from a measurement program designed to investigate the variations in sensitivity of focal plane arrays on a sub-pixel scale. High-resolution measurements have previously been reported for a front- illuminated CCD device. New measurements are now provided on the sensitivity variations with in a single pixel of a backside-illuminated CCD. The measurements were made using a stable broadband light source and two high-precision translation stages. The pixel scans have been performed using 4 different filters (3 broadband and 1 narrowband). The results for each spectral region are presented.19
Observations using the Starfire Optical Range (SOR) 1.5m telescope, located near Albuquerque, NM, were made during two separate observing runs, one in 1995 and the other in 1996. Image data was collected using a cooled 2K by 2K user provided CCD camera system. During the first observing sessions a standard SOR direct imaging configuration was used where a CCD imager. For the second observing run the configuration was modified to use a mirror with a small on- axis hole that allowed all the light in the central region to be used by the AO system while the remainder of the field was directed to the CCD. The data from these observations were used to investigate a number of issues related to AO observing including: (i) the effect of scattered laser light on image quality; (ii) the photometric accuracy across an AO corrected field; (iii) the PSF variations across an AO corrected field; (iv) the limits to observation of close companions using a mirror with a hole as a coronograph. The result of these observing runs are presented along with representative images obtained using no correction, partial correction, using natural guide stars, and Rayleigh laser beacon configuration.
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