  We present a new generation of chemically consistent evolutionary synthesis
models for galaxies of various spectral types from E through Sd. The models
follow the chemical enrichment of the ISM and take into account the increasing
initial metallicity of successive stellar generations using recently published
metallicity dependent stellar evolutionary isochrones, spectra and yields. Our
first set of closed-box 1-zone models does not include any spatial resolution
or dynamics. For a Salpeter initial mass function (IMF) the star formation
rate(SFR) and its time evolution are shown to successfully parameterise
spectral galaxy types E, ..., Sd. We show how the stellar metallicity
distribution in various galaxy types build up with time to yield after $\sim
12$ Gyr agreement with stellar metallicity distributions observed in our and
other local galaxies. The models give integrated galaxy spectra over a wide
wavelength range (90.9\AA - 160$\mu$m), which for ages of $\sim 12$ Gyr are in
good agreement not only with observed broad band colours but also with template
spectra for the respective galaxy types. Using filter functions for
Johnson-Cousins, as well as for HST broad band filters in the optical and
Bessel & Brett's NIR filter system, we calculate the luminosity and colour
evolution of model galaxies over a Hubble time. Including a standard
cosmological model and the attenuation by intergalactic hydrogen we present
evolutionary and cosmological corrections as well as apparent luminosities in
various filters over the redshift range from z $\sim 5$ to the present for our
galaxy types and compare to earlier models using single (=solar) metallicity
input physics only. We also present a first comparison of our cc models to HDF
data.(Abridged abstract)
