Far ultraviolet observations of the expanding shell in Eridanus

Details Far ultraviolet observations of the expanding shell in Eridanus Far ultraviolet observations of the expanding shell in Eridanus

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...124..300p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 124, no. 2, Aug. 1983, p. 300-308. Research supported by the Danish Space Boar

Astronomy and Astrophysics

Astronomy

13

Background Radiation, Far Ultraviolet Radiation, Interstellar Matter, Ultraviolet Astronomy, Fluorescence, Reflection Nebulae, Terrestrial Radiation, Thermal Emission, Zodiacal Light

Scientific paper

A thin strip of the sky near the south galactic pole has been observed in the 1350-1750 Å wavelength band. After correcting for hot stars in the instrument field of view, the measured count rates were found to vary smoothly from a minimum of ≅55 cs-1 near l = 30°, b = -60° to a maximum of ≅740 cs-1, in the direction of l = 199°, b = -49° corresponding to specific intensities between ≅600 and 8000 photons cm-2s-1sr-1Å-1, assuming a flat incident spectrum in this wavelength range. Near the edge of a prominent Hα filament in Eridanus, the measured intensities vary by ≅2500 photons cm-2s-1sr-1Å-1 over ≅6° in the sky. The magnitude and spatial variation of the observed signal is incompatible with any known source of terrestrial far UV airglow, zodiacal light, or with the expected emission of high latitude reflection nebulosities. Three alternative sources that, alone or together with reflection nebulae, might explain the high intensities in this region are H2 fluorescence emission by cool clouds, H I two photon emission from ionized gas, and thermal emission from a fast radiative shock. The required emission parameters are compatible with the observed characteristics of the expanding shell in Eridanus.

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