Galileo Ultraviolet Spectrometer experiment

Details Galileo Ultraviolet Spectrometer experiment Galileo Ultraviolet Spectrometer experiment

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ssrv...60..503h&link_type=abstract

Space Science Reviews (ISSN 0038-6308), vol. 60, no. 1-4, May 1992, p. 503-530.

Computer Science

30

Galileo Spacecraft, Jupiter Atmosphere, Jupiter Satellites, Satellite-Borne Instruments, Ultraviolet Spectrometers, Extreme Ultraviolet Radiation, Field Of View, Hydrogen Atoms, Upper Atmosphere

Scientific paper

The Galileo ultraviolet spectrometer experiment uses data obtained by the Ultraviolet Spectrometer (UVS) mounted on the pointed orbiter scan platform and from the Extreme Ultraviolet Spectrometer (EUVS) mounted on the spinning part of the orbiter with the field of view perpendicular to the spin axis. The UVS is a Ebert-Fastie design that covers the range 113-432 nm with a wavelength resolution of 0.7 nm below 190 and 1.3 nm at longer wavelengths. The UVS spatial resolution is 0.4 deg x 0.1 deg for illuminated disk observations and 1 deg x 0.1 deg for limb geometries. The EUVS is a Voyager design objective grating spectrometer, modified to cover the wavelength range from 54 to 128 nm with wavelength resolution 3.5 nm for extended sources and 1.5 nm for point sources and spatial resolution of 0.87 deg x 0.17 deg. The EUVS instrument will follow up on the many Voyager UVS discoveries, particularly the sulfur and oxygen ion emissions in the Io torus and molecular and atomic hydrogen auroral and airglow emissions from Jupiter. The UVS will obtain spectra of emission, absorption, and scattering features in the unexplored, by spacecraft, 170-432 nm wavelength region. The UVS and EUVS instruments will provide a powerful instrument complement to investigate volatile escape and surface composition of the Galilean satellites, the Io plasma torus, micro- and macro-properties of the Jupiter clouds, and the composition structure and evolution of the Jupiter upper atmosphere.

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