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We present a new method to compute the cosmic emissivity $\E_\nu$ andbackground intensity $J_\nu$. Our method is based entirely on data from quasarabsorption-line studies, namely, the comoving density of HI and the meanmetallicity and dust-to-gas ratio in damped Ly$\alpha$ galaxies. Theseobservations, when combined with models of cosmic chemical evolution, aresufficient to determine the comoving rate of star formation as a function ofredshift. From this, we compute $\E_\nu $ and $J_\nu$ using stellar populationsynthesis models. Our method includes a self-consistent treatment of theabsorption and reradiation of starlight by dust. In all of our calculations,the near-UV emissivity declines rapidly between $z\approx1$ and $z=0$, inagreement with estimates from the Canada-France Redshift Survey. The backgroundintensity is consistent with a wide variety of observational limits and with atentative detection at far-IR wavelengths.Comment: Single PS file, To appear in the 10 June 1996 issue of ApJ Letter

Cosmic Emissivity and Background Intensity from Damped Lyman-Alpha Galaxies