4.5 Space Telescope Imaging Spectrograph (STIS)

STIS uses two-dimensional detectors operating from the ultraviolet to the near infrared (1150-11,000Å) in support of a broad range of spectroscopic capabilities. STIS can be used to obtain spatially resolved, long-slit (or slitless) spectroscopy of the 1150-10,300Å range at low to medium spectral resolutions (R ~ 500 to 17,000) with first-order gratings. Echelle spectroscopy at medium and high (R ~ 30,000 and 110,000) resolutions covering broad spectral ranges of ~ 800 and 200Å, respectively, is available in the ultraviolet (1150-3100Å). STIS can also be used for deep optical and solar-blind ultraviolet imaging.

The three 1024 x 1024 pixel detectors supporting spectroscopy and imaging applications are as follows.

• A solar-blind CsI (FUV) Multi-Anode Microchannel Array (MAMA) with a plate scale of 0.024"/pixel and a 25" x 25" FOV is available from 1150 to 1700Å.
• A Cs₂Te (NUV) MAMA with a plate scale of 0.024"/pixel and a 25" x 25" FOV is available from 1600 to 3100Å.
• A CCD with a plate scale of 0.05"/pixel and a 52" x 52" FOV is available from ~2000 to 11,000Å.

The MAMA detectors support time resolutions down to 125 micro-sec in TIME-TAG mode, and the CCD can be cycled in ~20 sec with use of small subarrays. The CCD and the MAMAs also provide coronagraphic spectroscopy in the visible and ultraviolet. Coronagraphic CCD imaging is also supported.