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tokens: listed in Cols. 2 and 3, respectively. Column 4 shows the isotopic ratio, while Col. 5 gives the references for the different elements. Table 2 Elemental abundances for individual lines in the solar spectrum. Notes. Columns 26 list the single abundances for the different instruments and resolutions. Columns 7 and 8 show the median abundance values for MIKE spectra for the different observation runs and the one dispersion, respectively. The mean abundances are used as solar abundance for MIKE spectra observed in the run with (see Table 1 in Bensby et al. 2014 ) since no solar spectra is available in this setting. Col. 9 lists the solar abundances values from Asplund et al. (2009) . 2.2. Spectral line synthesis The spectral lines from the heavy neutron-capture elements are usually located in the blue regions of the visible spectrum. The blue region is very crowded with spectral lines and is especially so for metal-rich disk stars, meaning that blends from other species are frequent. The crowdedness of the blue spectral regions also makes the placement of the continuum difficult. In addition, heavy elements usually consist of several isotopes, and their spectral lines can be affected by hyperfine splitting (hfs). Therefore, to determine abundances from these lines, one has to use spectral line synthesis in order to accurately account for wavelength shifts of the different isotopes, hyperfine components, and other blending features. Table 1 lists the spectral lines that we use in this study. It shows the analyzed lines with the isotopic ratios of the elements, ionisation stages, wavelengths, and excitation potential, along with reference work where these details were gathered. For Sm and Nd, which suffer in large part from isotopic shifts and also hfs, we use data from Roederer et al. (2008) , for La we used hfs-only components from Ivans et al. (2006) since La has only one naturally-occurring isotope, and for Eu we used shift correction for isotopic and hfs substructures from Lawler et al. (2001) . However, some of the lines of the elements affected by hfs are treated as single lines because the wavelength splitting is small enough to be ignored. In our linelists the lines treated as single lines are La ii at 4748 Å, Nd ii at 5130 Å, and at 5319 Å, and Sm ii at 4523 Å, 4577 Å, and 4669 Å. All lines from Sr ii , Zr ii, and Ce ii lines are treated as single lines since there is no information available on their hyperfine structure and isotopic shifts or because they do not suffer from any of these problems. Atomic data for blending lines and other nearby lines were taken from the compilation available in the Vienna Atomic Line Database (VALD, Piskunov et al. 1995 ; Ryabchikova et al. 1997 ; Kupka et al. 1999 , 2000 ). The complete linelists with hyperfine components can be found in Appendix A . 2.3. Abundance determination The methodology for abundance determination is the same as in Battistini Bensby (2015) where we analyzed Sc, V, Mn, and Co for