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Presolar SiC grains formed around Asymptotic Giant Branch (AGB) stars during their carbon-rich phase and contain heavy elements in trace amounts showing the signature of the slow neutron capture process (s process). Thanks to recent advances in analysis techniques, SiC data now provide extremely precise information on neutron capture cross sections and AGB models. For example, high-precision data for Mo in single SiC grains indicate that a revision of the Mo neutron capture cross section is needed, while data for Zr indicates that the Ne(α,n)Mg reaction cannot be a dominant neutron source for the s process in AGB stars. We present model predictions for the composition of Fe-peak elements in AGB stars. These elements could be analysed in the near future thus providing further stringent constraints to our understanding of AGB stars.