FAR-ULTRAVIOLET EMISSION FROM THE TAURUS MOLECULAR CLOUD

Far-ultraviolet spectra of diffuse emission from a region in the Taurus molecular cloud are presented. These data were obtained with the Berkeley spectrometer on NASA's Ultraviolet Experiment (UVX) payload. The intensity of the continuum emission drops as the optical depth increases toward the denser part of the cloud, an effect which is the opposite of that observed for the diffuse flux at high galactic latitudes. At the center of the aperture, the optical depth is very large, and the continuum emission must be produced by backscattering. At the edges of the cloud, the continuum intensity rises by a factor of 2. The data are interpreted with a new radiative transfer model, which is significantly more sophisticated than its predecessors. If the grain scattering properties are constant across the cloud, a unique best-fit combination can be determined from the data. The best-fit albedo is 0.6 +/- 0.1 at 1600 angstrom. The best-fit value for the phase factor g is 0.5 +/- 0.15. The intensity of the fluorescence of H-2, combined with an upper limit to the column density of atomic hydrogen associated with the cloud, sets a lower limit of about 130 CM-3 to the density in the fluorescence region. Our estimate of the flux incident on the cloud at 1000 angstrom is a factor of 2 to 3 lower than the value required to produce the measured fluorescence intensity. Most mechanisms which might reconcile the discrepancy reduce the derived albedo and phase factor.