Radiative Transfer Analysis of Far‐Ultraviolet Background Observations Obtained with the Far Ultraviolet Space Telescope

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Abstract
In 1992, the Far Ultraviolet Space Telescope provided measurements of the ultraviolet (140-180 nm) diffuse sky background at high, medium, and low Galactic latitudes. A significant fraction of the detected radiation was found to be of Galactic origin, resulting from scattering by dust in the diffuse interstellar medium. To simulate the radiative transfer in the Galaxy, we employed a Monte Carlo model that utilized a realistic, nonisotropic radiation field based on the measured fluxes (at 156 nm) and positions of 58,000 TD-1 stars, and a cloud structure for the interstellar medium. The comparison of the model predictions with the observations led to a separation of the Galactic scattered radiation from an approximately constant background, attributed to airglow and extragalactic radiation, and to a well-constrained determination of the dust scattering properties. The derived dust albedo a = 0.45 ± 0.05 is substantially lower than albedos derived for dust in dense reflection nebulae and star-forming regions, while the phase function asymmetry g = 0.68 ± 0.10 is indicative of a strongly forward-directed phase function. We show the highly nonisotropic phase function to be responsible, in conjunction with the nonisotropic UV radiation field, for the wide range of observed correlations between the diffusely scattered Galactic radiation and the column densities of neutral atomic hydrogen. The low dust albedo is attributed to a size distribution of grains in the diffuse medium with average sizes smaller than those in dense reflection nebulae.
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