Speckle imaging with the MAMA detector: Preliminary results

Details Speckle imaging with the MAMA detector: Preliminary results Speckle imaging with the MAMA detector: Preliminary results

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106..992h&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 106, no. 703, p. 992-1002

Other

4

Angular Resolution, High Resolution, Image Reconstruction, Imaging Techniques, Microchannels, Optical Equipment, Phase Shift, Speckle Interferometry, Astronomical Interferometry, Binary Stars, Power Spectra, Quantum Efficiency, Sampling, Signal To Noise Ratios

Scientific paper

We report on the first successful speckle imaging studies using the Stanford University speckle interferometry system, an instrument that uses a multianode microchannel array (MAMA) detector as the imaging device. The method of producing high-resolution images is based on the analysis of so-called 'near-axis' bispectral subplanes and follows the work of Lohmann et al. (1983). In order to improve the signal-to-noise ratio in the bispectrum, the frame-oversampling technique of Nakajima et al. (1989) is also employed. We present speckle imaging results of binary stars and other objects from V magnitude 5.5 to 11, and the quality of these images is studied. While the Stanford system is capable of good speckle imaging results, it is limited by the overall quantum efficiency of the current MAMA detector (which is due to the response of the photocathode at visible wavelengths and other detector properties) and by channel saturation of the microchannel plate. Both affect the signal-to-noise ratio of the power spectrum and bispectrum.

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