The flat fielding and achievable signal-to-noise of the MAMA detectors

Details The flat fielding and achievable signal-to-noise of the MAMA detectors The flat fielding and achievable signal-to-noise of the MAMA detectors

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997hstc.work...29k&link_type=abstract

The 1997 HST Calibration Workshop with a New Generation of Instruments, p. 29

Computer Science

Performance

1

Hubble Space Telescope, Multi-Anode Microchannel Arrays, Signal To Noise Ratios, Calibrating, Spectrographs, Radiation Detectors, Imaging Spectrometers, Ultraviolet Spectroscopy, Ultraviolet Spectra, Performance Tests, Spectral Resolution, Spectral Bands, Image Reconstruction

Scientific paper

The Space Telescope Imaging Spectrograph (STIS) was designed to achieve a signal-to-noise (S/N) of at least 100:1 per resolution element. Multi-Anode Microchannel Arrays (MAMA) observations during Servicing Mission Orbital Verification (SMOV) confirm that this specification can be met. From analysis of a single spectrum of GD153, with counting statistics of approximately 165 a S/N of approximately 125 is achieved per spectral resolution element in the far ultraviolet (FUV) over the spectral range of 1280A to 1455A. Co-adding spectra of GRW+7OD5824 to increase the counting statistics to approximately 300 yields a S/N of approximately 190 per spectral resolution element over the region extending from 1347A to 1480A in the FUV. In the near ultraviolet (NUV), a single spectrum of GRW+7OD5824 with counting statistics of approximately 200 yields a S/N of approximately 150 per spectral resolution element over the spectral region extending from 2167 to 2520A. Details of the flat field construction, the spectral extraction, and the definition of a spectral resolution element will be described in the text.

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