  We study the effects of neutron captures in AGB stars on \oq Fe-group\cqb
elements, with an emphasis on Cr, Fe, and Ni. These elements show anomalies in
$^{54}$Cr, $^{58}$Fe, and $^{64}$Ni in solar-system materials, which are
commonly attributed to SNe. However, as large fractions of the interstellar
medium (ISM) were reprocessed in AGB stars, these elements were reprocessed,
too. We calculate the effects of such reprocessing on Cr, Fe, and Ni through
1.5\msb and 3\msb AGB models, adopting solar and 1/3 solar metallicities. All
cases produce excesses of $^{54}$Cr, $^{58}$Fe, and $^{64}$Ni, while the other
isotopes are little altered; hence, the observations may be explained by AGB
processing. The results are robust and not dependent on the detailed initial
isotopic composition. Consequences for other \oq Fe group\cqb elements are then
explored. They include $^{50}$Ti excesses, and some production of
$^{46,47,49}$Ti. In many circumstellar condensates, Ti quantitatively reflects
these effects of AGB neutron captures. Scatter in the data results from small
variations (granularity) in the isotopic composition of the local ISM. For Si,
the main effects are instead due to variations in the local ISM from different
SNe sources. The problem of Ca is discussed, particularly with regard to
$^{48}$Ca. The measured data are usually represented assuming terrestrial
values for $^{42}$Ca/$^{44}$Ca. Materials processed in AGB stars or sources
with variable initial $^{42}$Ca/$^{44}$Ca ratios can give apparent $^{48}$Ca
excesses/deficiencies, attributed to SNe. The broader issue of Galactic
Chemical Evolution is also discussed in view of the isotopic granularity in the
ISM. \end{abstract}
