The Infrared Spectral Energy Distribution of Normal Star-Forming Galaxies: Calibration at Far-Infrared and Submillimeter Wavelengths

New far-infrared and submillimeter data are used to solidify and to extend to long wavelengths the empirical calibration of the infrared spectral energy distribution (SED) of normal star-forming galaxies. As was found by Dale et al. (2001), a single parameter family, characterized by fν(60μm) fν(100μm) , is adequate to describe the range of normal galaxy spectral energy distributions observed by IRAS and ISO from 3 to 100 μm. However, predictions based on the first generation models at longer wavelengths (122 to 850 μm) are increasingly overluminous compared to the data for smaller fν(60μm) fν(100μm) , or alternatively, for weaker global interstellar radiation fields. After slightly modifying the far-infrared/submillimeter dust emissivity in those models as a function of the radiation field intensity to better match the long wavelength data, a suite of SEDs from 3 μm to 20 cm in wavelength is presented. Results from relevant applications are also discussed, including submillimeter-based photometric redshift indicators, the infrared energy budget and simple formulae for recovering the bolometric infrared luminosity, and dust mass estimates in galaxies. Regarding the latter, since galaxy infrared SEDs are not well-described by single blackbody curves, the usual methods of estimating dust masses can be grossly inadequate. The improved model presented herein is used to provide a more accurate relation between infrared luminosity and dust mass. Subject headings: dust, extinction — galaxies: general — galaxies: ISM — infrared: galaxies — infrared: ISM: continuum