  We extend our spiral galaxy models that successfully describe nearby template
spectra as well as the redshift evolution of CFRS and HDF spirals to include -
in a chemically consistent way - the redshift evolution of a series of
individual elements. Comparison with observed DLA abundances shows that DLAs
might well be the progenitors of present-day spiral types Sa through Sd. Our
models bridge the gap between high redshift DLA and nearby spiral HII region
abundances. The slow redshift evolution of DLA abundances is a natural
consequence of the long SF timescales for disks, the scatter at any redshift
reflects the range of SF timescales from early to late spiral types. We claim
that while at high redshift all spiral progenitor types seem to give rise to
DLA absorption, towards low redshifts, the early type spirals seem to drop out
of DLA samples due to low gas and/or high metal and dust content. Model
implications for the spectrophotometric properties of the DLA galaxy population
are discussed in the context of campaigns for the optical identifications of
DLA galaxies both at low and high redshift.
