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Session 43 - HST Instruments & Other Missions.
Display session, Tuesday, January 14
Metropolitan Ballroom,

[43.04] Pre-Flight Calibration Results for the Space Telescope Imaging Spectrograph I. Overview

M. Kaiser (JHU), C. Bowers, T. Gull, S. Heap, R. Kimble, B. Woodgate (GSFC), S. Kraemer (CSC/CUA), G. Hartig (STScI), J. Valenti (JILA), S. Downey, D. Ebbets, D. Hood (BATC), K. Feggans (ACC/GSFC), N. Collins, W. Landsman, E. Malamuth (HSTX/GSFC)

The Space Telescope Imaging Spectrograph (STIS) is a second generation Hubble Space Telescope instrument. STIS will be installed in HST during the second servicing mission in February 1997.

The STIS instrument provides both spectrographic and imaging capability from the far ultraviolet (1150 Åthrough the visible (10000 Åregion of the spectrum. The far ultraviolet (Band 1) spans the wavelengths from 1150 Å\ to 1700 Å\ and utilizes a MAMA detector with a CsI photocathode. The near ultraviolet (Band 2) spans the wavelengths from 1650 Å\ to 3100 Å\ and is supported by a MAMA detector with a CsTe photocathode. Band 3 spans the wavelengths from 3050 Å\ to 5550 Å\ and Band 4 spans the wavelength region from 5500 Å\ to 11000 ÅBoth visible bands are supported by the same CCD detector. Multiple resolutions are supported for each band. Low and medium resolution, first order spectroscopy, is provided from the far ultraviolet through the visible region of the spectrum for faint objects. In addition, high resolution echelle spectroscopy is provided for both ultraviolet bands. For the ultraviolet bands the field-of-view is 27 arcseconds and for the visible bands the field-of-view is 52 arcseconds.

The results of the ground based calibration of STIS will be presented. Both wavelength and flat field calibrations are supported through the use of on-board calibration lamps. In particular, sensitivity and throughput measurements of the various STIS modes will be discussed. Both ``supported'' and ``available'' modes will also be identified and discussed.

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