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Althought this Meeting is devoted to the discussion of the nature of the Ultraluminous Far-IR Galaxies at low and high redshift, and their role in galaxy evolution, I will not directly tackle this topic in my presentation. I will instead summarize and discuss the properties of a complementary sample of galaxies: the high-z (z > 2), UV-bright systems ([30], [31]). The number of known z > 2 galaxies is now large enough that they can be classified as a population, and have been used to infer the past star formation history of the Universe ([22], [23]). As with all statistical studies, observational incomplenetesses and selection biases are a concern. In the case of the high-z population, volume corrections, luminosity selections and, last but potentially the most important, dust obscuration effects have been discussed by a number of authors (e.g., [24], [3], [27], [31], [5]). Here I will highlight the impact of dust obscuration on the high-z galaxies and the inferred star formation history. I hope in this way to set a ground for comparison of the high-z UV-bright galaxy population with the high-z Ultraluminous Far-IR galaxies recently discovered with SCUBA ([28], [17], [2], [10]; see also the contributions of I. Smail, of A. Blain, and of M. Rowan-Robinson to these Proceedings).