  This is a summary of arguments in favor of observing high-redshift star
formation in the UV as presented at the Ringberg meeting in September 2000. The
most rapidly star-forming galaxies are very dusty, easier to detect at 850um
than in the UV, but less rapidly star-forming galaxies are less obscured by
dust and as a result the comparatively faint galaxies that hosted most
high-redshift star formation are easiest to detect in the UV. The correlation
of star-formation rate and dust obscuration implies that extremely luminous
dusty galaxies are usually as bright in the UV as the less luminous dust-free
galaxies, and that any UV survey at a given redshift 0<z<~3 deep enough to
detect the majority of the UV luminosity density will detect the majority of
IR-selected galaxies as well. Little star formation occurs in galaxies that are
completely hidden from UV surveys. I review recent attempts to estimate
star-formation rates for high-redshift galaxies from UV data alone. The
strength of UV surveys is that they detect large numbers of high-redshift
galaxies, even ones that are intrinsically very faint, in large and
representative comoving volumes. The weakness is that star-formation rates are
difficult to estimate for the detected galaxies. IR surveys complement them
perfectly: star-formation rates can be estimated with reasonable confidence,
but only small regions of the sky can be surveyed and only the most luminous
sources can be detected. Multiwavelength cooperation, not conflict, will lead
to future progress in this field.
