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We introduce a new empirical function for modeling the spectral energydistributions of galaxies. We apply it to a sample of 590 galaxies in theregion of the HDF with $z < 1.5$ using multi-color photometry with widewavelength coverage combined with spectroscopic redshifts from our 93% completeR-selected redshift survey there. We find the following: As expected, galaxieswith strong signs of recent star formation (i.e. those which show emissionlines) have bluer continua in both the rest frame UV and theoptical/near-infrared. The redder galaxies tend to be more luminous. The SEDsof actively star forming galaxies become bluer in the mean in the rest-frame UVat higher redshift, which trend might arise from SED modeling errors. Asidefrom this, we discern no change with redshift in the relationship between SEDcharacteristics and galaxy spectral type based on the strength of narrowemission and absorption features. There is no evidence in our R-selected samplethat supports the existence of a substantial population of very dusty starforming galaxies at z < 1.5. The overall pattern of the L(K) - z relationshipsuggests that passive evolution at constant stellar mass is a goodapproximation to the actual behavior of at least the most luminous galaxies inthis large sample of galaxies in the region of the HDF out to z \sim 1.5.(abridged)Comment: Minor changes in text and addition of one figure to conform to  version accepted for publication in the Astronomical Journal (June 2001  issue

Caltech Faint Galaxy Redshift Survey. XIII. Spectral Energy Distributions for Galaxies in the Region of the Hubble Deep Field North*