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This paper examines what can be learned about high-redshift star formationfrom the small fraction of high-redshift galaxies' luminosities that is emittedat accessible wavelengths. We review and quantify empirical correlationsbetween bolometric luminosities produced by star formation and the UV, mid-IR,sub-mm, and radio luminosities of galaxies in the local universe. Thesecorrelations suggest that observations of high-redshift galaxies at any ofthese wavelengths should constrain their star-formation rates to within0.2--0.3 dex. We assemble the limited evidence that high-redshift galaxies obeythese locally calibrated correlations. The characteristic luminosities and dustobscurations of galaxies at z ~ 0, z ~ 1, and z ~ 3 are reviewed. Afterdiscussing the relationship between the high-redshift populations selected insurveys at different wavelengths, we calculate the contribution to the 850umbackground from each. The available data show that a correlation betweenstar-formation rate and dust obscuration L_dust/L_UV exists at low and highredshift. This correlation plays a central role in the major conclusion of thispaper: most star formation at high redshift occurred in galaxies with 1 <L_dust/L_UV < 100 similar to those that host the majority of star formation inthe local universe and to those that are detected in UV-selected surveys.(abridged)Comment: Scheduled for publication in ApJ v544 Dec 2000. Significant changes  to section 4. Characteristic UV and dust luminosities of star-forming  galaxies at redshifts z~0, z~1, and z~3 presented. Existence of extremely  obscured galaxies more clearly acknowledged. Original conclusions reinforced  by the observed correlation between bolometric luminosity and dust  obscuration at 0<z<

Multiwavelength Observations of Dusty Star Formation at Low and High Redshift