TEMPLATE ULTRAVIOLET TO NEAR-INFRARED SPECTRA OF STAR-FORMING GALAXIES AND THEIR APPLICATION TO K-CORRECTIONS

Template UV-optical spectra of quiescent and starburst galaxies are pr esented and used to derive K-corrections as a function of morphologica l type and redshift. IUE observations and archival data are used for t he UV template spectra. The optical spectra are from ground-based obse rvations obtained in apertures that match closely the 200 arcsec(2) IU E aperture. The templates of quiescent galaxies are built according to morphological type, elliptical, bulge, SO, Sa, Sb, and Sc, and the te mplates of starburst galaxies according to color excess. The unprecede nted characteristics of these templates is that UV and optical spectra have been obtained in matched apertures to produce consistent spectra l information from 1200 to 10,000 Angstrom Despite the relatively smal l IUE aperture, the galaxy stellar populations are well represented in the elliptical, SO, Sa, and Sc, and in the starburst templates. The s pectra are available digitally. The UV-optical templates can be applie d to the classification of high-redshift galaxies and to the identific ation of the host galaxies of quasars. The templates predict that obse rved magnitudes from traditional ground-based photometric surveys can be uniquely interpreted, For example, U, B, and I magnitudes uniquely determine both the redshift and the morphological type of a galaxy. Th e template spectra are also used to calculate K-corrections for galaxi es as a function of morphological type and redshift, up to z = 2. Thes e improved K-corrections are not sufficient to explain the excess coun ts in faint blue galaxies. A subset of our galaxy templates are linked with published data from the radio to the X-ray for galaxies and quas ars. A comparison between the quiescent galaxies and the quasars sugge sts that, in the optical band, the host galaxy is a factor of 10-100 f ainter in flux than the quasar.