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 Dl ~ 800 or 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 coronographic spectroscopy in the visible and ultraviolet. Coronographic CCD imaging is also supported.
Space telescope Science Institute http://www.stsci.edu |