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We redetermine the abundances of all iron group nuclei in the Sun, based onneutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solarspectrum. We employ a realistic 3D hydrodynamic model solar atmosphere,corrections for departures from local thermodynamic equilibrium (NLTE),stringent line selection procedures and high quality observational data. Wehave scoured the literature for the best quality oscillator strengths,hyperfine constants and isotopic separations available for our chosen lines. Wefind $\log \epsilon_\mathrm{Sc}=3.16\pm0.04$, $\log\epsilon_\mathrm{Ti}=4.93\pm0.04$, $\log \epsilon_\mathrm{V}=3.89\pm0.08$,$\log \epsilon_\mathrm{Cr}=5.62\pm0.04$, $\log\epsilon_\mathrm{Mn}=5.42\pm0.04$, $\log \epsilon_\mathrm{Fe}=7.47\pm0.04$,$\log \epsilon_\mathrm{Co}=4.93\pm0.05$ and $\log\epsilon_\mathrm{Ni}=6.20\pm0.04$. Our uncertainties factor in both statisticaland systematic errors (the latter estimated for possible errors in the modelatmospheres and NLTE line formation). The new abundances are generally in goodagreement with the CI meteoritic abundances but with some notable exceptions.This analysis constitutes both a full exposition and a slight update of thepreliminary results we presented in Asplund, Grevesse, Sauval & Scott(arXiv:0909.0948), including full line lists and details of all input data weemployed.

The elemental composition of the Sun II. The iron group elements Sc to Ni