A long-slit far-ultraviolet spectrum (1250-1850 Γ
) of Comet Austin ( (1990 \mathrm{~V}) ) was obtained from a sounding rocket experiment launched on 21 April 1990. Emissions of (\mathrm{OI}, \mathrm{CI}, \mathrm{SI}), and (\mathrm{CO}) were detected during the (270 \mathrm{sec}) of data acquisition. The spectral resolution was (5.5 \AA), while the spatial resolution was limited by pointing jitter to (\sim 30) arcsec. The spatial profiles of the carbon and oxygen emissions show narrow enhancements which are suggestive of a cometary outburst which occurred (15-20 \mathrm{hr}) before the observation. The spatial distribution of the atomic carbon is similar to that measured during two observations of Comet P/Halley (1986 III) and, as in the case of Halley, is not well matched by current models of (\mathrm{CO}) photodissociation. The (\mathrm{CO}) profile, for cometocentric distances greater than (10^{4} \mathrm{~km}), is that of a parent molecule evaporating directly from the nucleus with a production rate of (4.0 \pm) (1.3 \times 10^{27}) molecules (\mathrm{sec}^{-1}). The OI (\lambda 1304) emission, also similar in spatial distribution to that observed in Halley, includes a contribution due to Bowen fluorescence induced by solar HI Lyman- (\beta), and its distribution can be understood as that due to the photodissociation of (\mathrm{H}{2} \mathrm{O}), with a production rate of (6.2 \pm 3.3 \times 10^{28}) molecules (\mathrm{sec}^{-1}). The abundance of (\mathrm{CO}), relative to water, is (6.5 \pm 4.0 %). The spatial profile of SI (\lambda 1814) was also obtained, and is consistent with that of a daughter product of short-lived species such as (\mathrm{CS}{2}) and (\mathrm{H}_{2} \mathrm{~S}), with a total production rate of (6.0 \pm 1.9 \times 10^{26}) molecules (\mathrm{sec}^{-1}). (c) 1993 Academic Press. Inc.