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The Space Telescope Imaging Spectrograph (STIS) is a second-generation scientific instrument for the Hubble Space Telescope (HST), currently scheduled for in-orbit installation onto the HST in 1997. STIS will cover the wavelength range from 115 to 1000 nm in a variety of spectroscopic modes with resolutions ranging from 30 to 100,000. The use of two-dimensional detectors (1024 x 1024 pixels), in contrast to the linear array detectors used by the first generation HST spectrographs, will permit STIS to extend the capabilities of HST to long-slit imaging spectroscopy and high resolution echelle spectroscopy with wide simultaneous wavelength coverage.
For coverage of the 305-1000 nm region, STIS will employ a custom CCD detector which has been developed at Scientific Imaging Technologies (SITe, formerly Tektronix). This backside-illuminated device incorporates a proprietary SITe backside treatment and anti-reflective coating to extend the useful quantum efficiency shortward of 305 nm. It also features low noise amplifiers, multi-pinned-phase implants for low dark current and radiation tolerance, minichannel implants for improved charge transfer efficiency at low signal levels, and four quadrant readout for operational flexibility and reliability. The thermo-electrically cooled CCD will be flown in a sealed, evacuated housing with its exterior at room temperature to minimize the condensation of absorbing contaminants in orbit.
Fabrication of flight-candidate CCDs is currently underway at SITe. An engineering model CCD housing and readout electronics set are nearing completion at Ball Aerospace. Performance results for these components along with results of CCD radiation testing will be presented.
