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tokens: Table A.1 Linelists for the synthesis of Sr. Notes. The lists include atomic data for Sr from Bautista et al. (2002) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.2 Linelists for the synthesis of Zr. Notes. The lists include atomic data for Zr from Ljung et al. (2006) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.3 Linelists for the synthesis of La. Notes. The lists include the hfs (when available) of the La in question taken from Ivans et al. (2006) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.4 Linelists for the synthesis of Ce. Notes. The lists include atomic data for Ce from Lawler et al. (2009) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.5 Linelists for the synthesis of Nd. Notes. The lists include the hfs (when available) of the Nd in question taken from Roederer et al. (2008) and additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.6 Linelists for the synthesis of Sm. Notes. The lists include the hfs (when available) of the Sm in question taken from Lawler et al. (2006) and Roederer et al. (2008) , as well as additional lines nearby. Columns represent element line, wavelength, and log() values. Table A.7 Linelists for the synthesis of Eu ii . Notes. The lists include the hfs of the Eu ii in question taken from Lawler et al. (2001) and additional lines nearby. Columns represent element line, wavelength, and log() values. Appendix B: Solar abundance plots Figures B.1 – B.5 show the synthesis for all the lines analyzed in this work for the solar spectrum from Vesta observed at Magellan in January 2006. Each plot shows (in the bigger panel) the line fitting with the best fit to the observed one and the different abundances in steps of 0.04 dex. In the lower panel, the differences between the observed spectrum and the synthetic one are shown, with the difference with the best fit highlighted. In the small square panel, the values for the different abundances are represented, with the red dot representing the minimum, hence the best fit value for the elemental abundance. Fig. B.1 Solar spectrum taken using asteroid Vesta during the run at Magellan in January 2006. Spectral lines are listed in order of element and wavelength. Chemical elements with all the hfs lines are indicated inside the lines. The different colored lines represent the different synthetic spectra with different abundances in steps of 0.04 dex, while the dots are the observed spectra. The lower panels show the values of differences between the real and synthetic spectra for the synthetic spectra plotted above. The red lines represent the best fit derived from un-normalized , visible in the small plot as a red dot. Here the fits for the Sr line and the five Zr lines are shown. Fig. B.2 As in Fig. B.1 but for the four