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The comoving luminosity density of the Universe is estimated from the CFRSfaint galaxy sample in three wavebands (2800A, 4400A and 1 micron) over theredshift range 0 < z < 1. In all three wavebands, the comoving luminositydensity increases markedly with redshift. For a (q_0 = 0.5, Omega = 1.0)cosmological model, the comoving luminosity density increases as $(1+z)^{2.1\pm 0.5}$ at 1 micron, as $(1+z)^{2.7 \pm 0.5}$ at 4400A and as $(1+z)^{3.9 \pm0.75}$ at 2800A, these exponents being reduced by 0.43 and 1.12 for (0.05,0.1)and (-0.85,0.1) cosmological models respectively. The variation of theluminosity density with epoch can be reasonably well modelled by an activelyevolving stellar population with a Salpeter initial mass function (IMF)extending to 125 M_sun, a star-formation rate declining with a power 2.5, and aturn-on of star-formation at early epochs. A Scalo (1986) IMF extending to thesame mass limit produces too many long-lived low mass stars. This rapidevolution of the star-formation rate and comoving luminosity density of theUniverse is in good agreement with the conclusions of Pei and Fall (1995) fromtheir analysis of the evolving metallicity of the Universe. One consequence ofthis evolution is that the physical luminosity density at short wavelengths hasprobably declined by two orders of magnitude since z ~ 1.

The Canada-France Redshift Survey: The Luminosity Density and Star Formation History of the Universe to [ITAL]z[/ITAL] ∼ 1