Space Telescope Imaging Spectrograph (STIS) is a versatile "combi-instrument"
taking advantage of modern technologies. It combines a camera with a spectrograph,
and covers a wide range of wavelengths from the near-infrared region into
the ultraviolet. A spectrograph spreads out the light gathered by a telescope
so that it can be analyzed to determine such properties of celestial objects
as chemical composition and abundances, temperature, radial velocity, rotational
velocity, and magnetic fields. Its spectrograph can be switched between two
different modes of usage: 1.So-called "long slit spectroscopy" where spectra
of many different points across an object are obtained simultaneously. 2.So-called
"echelle spectroscopy" where the spectrum of one object is spread over the
detector giving better wavelength resolution in a single exposure. STIS also
has a so-called coronograph which can block light from bright objects, and
in this way enables investigations of nearby fainter objects.
||Camera and Spectrograph
||2.2 x 0.9 x 0.9 m
|Field of view
||MAMA - 25 x 25 arcseconds
CCD - 50 x 50 arcseconds
||1150 to 10000 Angstroms
The Space Telescope Imaging Spectrograph (STIS).
A STIS spectrum of the galaxy NGC 4151 revealing that gas is flowing out of a black hole in its center.
STIS image of stars in the elliptical galaxy NGC 205 together with stars
in the foreground from our own Milky Way. Image: STIS parallel program. Image
reduction: Phil Plait.