All Tables

Table 1: Ionization equilibria between Fe I and Fe II, and between Co I and Co II. Each abundance was given for two model atmospheres.
Table 2: Analyses of individual atomic lines. Columns from left to right are: the names of ion, wavelength in Å, excitation potential ( $\chi$ ) in eV, log gf value, reference for log gf, log $\epsilon$ , the remark (HFS : the abundances determined by adopting the HFS data taken from Kurucz 2001). The full table is available in electronic form at the CDS.
Table 3: Elemental abundances in HR 5049. Consecutive columns are as follows: the name of ion, the number of used lines, the derived abundance, the standard deviation, the solar log $\epsilon$ , and the logarithmic abundance for HR 5049 relative to the Sun.
Table 4: Abundance changes for each ion in HR 5049. $\Delta M$ : the abundance difference due to the change of the metallicity from [M/H] = 1.0 to 0.0. $\Delta T$ +: $T_{\rm eff}=10~300$ K + 300 K (increase $T_{\rm eff}$ by 300 K), $\Delta T$ -: $T_{\rm eff}=10~300$ K - 300 K, $\Delta G$ +: log g = 3.81 + 0.2, and $\Delta G-$ : log g = 3.81 - 0.2.
Table 5: Comparison of elemental abundances in HR 5049 with three CP2 stars.