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Table 4

Average abundances implied by all lines of elements from Cu to Th.

Species 3D ⟨3D⟩ HM marcs miss 3D-HM 3D-⟨3D⟩ Recommended Meteoritic
log ϵCu Cu i 4.18 ± 0.05 4.16 4.21 4.11 4.18 −0.03 0.02 4.18 ± 0.05 4.25 ± 0.04
log ϵZn Zn i 4.56 ± 0.05 4.52 4.53 4.46 4.54 0.03 0.04 4.56 ± 0.05 4.63 ± 0.04
log ϵGa Ga i 3.02 ± 0.05 3.00 3.09 2.96 3.02 −0.06 0.02 3.02 ± 0.05 3.08 ± 0.02
log ϵGe Ge i 3.63 ± 0.07 3.55 3.62 3.51 3.57 0.01 0.09 3.63 ± 0.07 3.58 ± 0.04
log ϵKr Interpolated s-process production rate (AGSS09) 3.25 ± 0.06 −2.27
log ϵRb Rb i 2.47 ± 0.07 2.52 2.57 2.48 2.54 −0.10 −0.04 2.47 ± 0.07 2.36 ± 0.03
log ϵSr Sr i 2.80 ± 0.06 2.82 2.84 2.77 2.79 −0.03 −0.01
Sr ii 2.85 ± 0.11 2.75 2.86 2.70 2.86 −0.01 0.09
Sr all 2.83 ± 0.06 2.78 2.85 2.73 2.83 −0.02 0.05 2.83 ± 0.06 2.88 ± 0.03
log ϵY Y ii 2.21 ± 0.05 2.17 2.20 2.14 2.20 0.01 0.04 2.21 ± 0.05 2.17 ± 0.04
log ϵZr (Zr i ) 2.57 ± 0.12 2.67 2.75 2.64 2.69 −0.18 −0.10
Zr ii 2.59 ± 0.04 2.55 2.59 2.53 2.59 −0.00 0.03 2.59 ± 0.04 2.53 ± 0.04
log ϵNb Nb ii 1.47 ± 0.06 1.49 −0.03 0.00 1.47 ± 0.06 1.41 ± 0.04
log ϵMo Mo i 1.88 ± 0.09 1.96 2.04 1.93 1.98 −0.16 −0.08 1.88 ± 0.09 1.94 ± 0.04
log ϵRu Ru i 1.75 ± 0.08 1.82 1.91 1.80 1.84 −0.17 −0.08 1.75 ± 0.08 1.76 ± 0.03
log ϵRh Rh i 0.89 ± 0.08 0.98 1.07 0.95 0.99 −0.17 −0.08 0.89 ± 0.08 1.06 ± 0.04
log ϵPd Pd i 1.55 ± 0.06 1.52 1.61 1.49 1.54 −0.06 0.03 1.55 ± 0.06 1.65 ± 0.02
log ϵAg Ag i 0.96 ± 0.10 0.95 1.04 0.92 0.96 −0.08 0.01 0.96 ± 0.10 1.20 ± 0.02
log ϵCd Cd i 1.77 ± 0.15 1.76 1.79 1.73 1.79 −0.03 0.01 1.77 ± 0.15 1.71 ± 0.03
log ϵIn In i Sunspot (Vitas et al. 2008) 0.80 ± 0.20 0.76 ± 0.03
log ϵSn Sn i 2.02 ± 0.10 2.06 2.13 2.04 2.09 −0.11 −0.05 2.02 ± 0.10 2.07 ± 0.06
log ϵXe Interpolated s-process production rate (AGSS09) 2.24 ± 0.06 −1.95
log ϵBa Ba ii 2.25 ± 0.07 2.15 2.18 2.10 2.17 0.07 0.10 2.25 ± 0.07 2.18 ± 0.03
log ϵLa La ii 1.11 ± 0.04 1.14 −0.03 0.00 1.11 ± 0.04 1.17 ± 0.02
log ϵCe Ce ii 1.58 ± 0.04 1.61 −0.03 0.01 1.58 ± 0.04 1.58 ± 0.02
log ϵPr Pr ii 0.72 ± 0.04 0.76 −0.04 −0.01 0.72 ± 0.04 0.76 ± 0.03
log ϵNd Nd ii 1.42 ± 0.04 1.45 −0.03 0.00 1.42 ± 0.04 1.45 ± 0.02
log ϵSm Sm ii 0.95 ± 0.04 0.99 −0.04 −0.01 0.95 ± 0.04 0.94 ± 0.02
log ϵEu Eu ii 0.52 ± 0.04 0.55 −0.03 0.00 0.52 ± 0.04 0.51 ± 0.02
log ϵGd Gd ii 1.08 ± 0.04 1.11 −0.03 0.01 1.08 ± 0.04 1.05 ± 0.02
log ϵTb Tb ii 0.31 ± 0.10 0.28 −0.04 −0.00 0.31 ± 0.10 0.32 ± 0.03
log ϵDy Dy ii 1.10 ± 0.04 1.13 −0.03 0.00 1.10 ± 0.04 1.13 ± 0.02
log ϵHo Ho ii 0.48 ± 0.11 0.51 −0.03 0.00 0.48 ± 0.11 0.47 ± 0.03
log ϵEr Er ii 0.93 ± 0.05 0.96 −0.03 0.01 0.93 ± 0.05 0.92 ± 0.02
log ϵTm Tm ii 0.11 ± 0.04 0.14 −0.03 0.01 0.11 ± 0.04 0.12 ± 0.03
log ϵYb Yb ii 0.85 ± 0.11 0.86 −0.01 0.03 0.85 ± 0.11 0.92 ± 0.02
log ϵLu Lu ii 0.10 ± 0.09 0.12 −0.02 0.00 0.10 ± 0.09 0.09 ± 0.02
log ϵHf Hf ii 0.85 ± 0.05 0.88 −0.03 0.00 0.85 ± 0.05 0.71 ± 0.02
log ϵW W i 0.83 ± 0.11 1.03 −0.19 −0.09 0.83 ± 0.11 0.65 ± 0.04
log ϵOs Os i 1.40 ± 0.05 1.41 1.50 1.40 1.44 −0.09 −0.01 1.40 ± 0.05 1.35 ± 0.03
log ϵIr Ir i 1.42 ± 0.07 1.40 1.46 1.38 1.43 −0.04 0.02 1.42 ± 0.07 1.32 ± 0.02
log ϵAu Au i 0.91 ± 0.08 0.89 0.93 0.88 0.93 −0.02 0.02 0.91 ± 0.08 0.80 ± 0.04
log ϵTl Tl i Sunspot (Lambert et al. 1972) 0.9 ± 0.2 0.77 ± 0.03
log ϵPb Pb i 1.92 ± 0.08 1.97 2.05 1.95 2.00 −0.14 −0.06 1.92 ± 0.08 2.04 ± 0.03
log ϵTh Th ii 0.03 ± 0.10 0.03 0.07 0.02 0.06 −0.04 −0.00 0.03 ± 0.10 0.06 ± 0.03

Notes. Abundances are given as the weighted mean across all lines in the given list, taking into account NLTE corrections for Zn i, Sr i, Sr ii, Ba ii, Eu ii, Pb i and Th ii. Zr i is shown in brackets because we do not consider this result reliable enough to include in our final adopted abundance. Note that because all means were computed using abundances accurate to three decimal places, entries in Cols. 8 and 9 differ in some cases from the differences between the entries in Cols. 3−5. We also give our final recommended solar photospheric abundance of each element, compared with the abundance in CI chondritic meteorites (Lodders et al. 2009, normalised to the silicon abundance determined in Paper I).

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