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Session 42 - Orfeus & STIS.
Display session, Wednesday, June 11
South Main Hall,

[42.07] In-Flight Detector Performance of the Space Telescope Imaging Spectrograph

R. Kimble (GSFC), V. Argabright, C. Van Houten, D. Dorn (BATC), M. Blouke (SITe), S. Kraemer (CUA), A. Danks (HSTX), P. Goudfrooij, M. Clampin (STScI), T. Beck (ACC), E. Malumuth, W. Landsman, R. J. Hill (HSTX), M. Kaiser (JHU), C. Bowers (GSFC), G. Hartig, J. Hayes, S. Baum, R. Bohlin, H. Ferguson, C. Leitherer (STScI), J. Feggans, J. Sandoval (ACC)

The Space Telescope Imaging Spectrograph (STIS), installed in the Hubble Space Telescope in February 1997, incorporates three array detectors to observe the wavelength range of 115 to 1000 nm in a versatile combination of spectroscopic and imaging modes. Ultraviolet wavelengths are covered by two photon-counting Multi-Anode Microchannel Array (MAMA) detectors developed by Ball Aerospace Technologies Corporation; these detectors are read out in a 2048 x 2048 image format. Near-UV and visible wavelengths are covered by a 1024 x 1024, UV-enhanced, backside-illuminated CCD developed by Scientific Imaging Technologies.

In-flight characterization of the performance of these detectors is well underway. We report here on the performance measured for these detectors in areas such as sensitivity, resolution, noise, linearity, flat field behavior, stability, dark current, and dynamic range.

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