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000002125 005__ 20160706150334.0
000002125 0247_ $$2DOI$$a10.1051/0004-6361/201424110
000002125 037__ $$aASTROimport-282
000002125 100__ $$aScott, P.
000002125 245__ $$aThe elemental composition of the Sun. II. The iron group elements Sc to Ni
000002125 260__ $$c2015
000002125 520__ $$aWe redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log ɛSc = 3.16 ± 0.04, log ɛTi = 4.93 ± 0.04, log ɛV = 3.89 ± 0.08, log ɛCr = 5.62 ± 0.04, log ɛMn = 5.42 ± 0.04, log ɛFe = 7.47 ± 0.04, log ɛCo = 4.93 ± 0.05 and log ɛNi = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA, 47, 481), including full line lists and details of all input data we employed. Tables 1-3 are available in electronic form at http://www.aanda.org
000002125 700__ $$aAsplund, M.
000002125 700__ $$aGrevesse, N.
000002125 700__ $$aBergemann, M.
000002125 700__ $$aSauval, A. J.
000002125 773__ $$cA26$$pAstronomy and Astrophysics$$v573$$y2015
000002125 85642 $$ahttp://esoads.eso.org/abs/2015A%26A...573A..26S
000002125 905__ $$apublished in
000002125 980__ $$aREFERD