All Tables

Table 1: Atomic constants for the Ru I and Hf II lines used in this work, and references for $\log gf$ . "Sun'' denotes the gf-values fitted on the solar and Arcturus spectra. Other gf-values were taken from VALD, Lundqvist et al. (2006) (L06), and Lawler et al. (2007) (L07).
Table 2: Uncertainties on abundances. $\log{A_{pf}}$ : output with the atmospheric parameters adopted; $\log{A_{pT}}$ : output by altering 1 $\sigma$ on adopted $T\rm _{eff}$ ; $\log{A_{pmt}}$ : output by altering 1 $\sigma$ on adopted metallicity; $\log{A_{pl}}$ : output by altering 1 $\sigma$ on adopted $\log g$ ; $\log{A_{p\xi}}$ : output by altering 1 $\sigma$ on adopted microturbulent velocity $\xi$ ; $\sigma _l$ : $\sigma_{\log\epsilon}$ , the uncertainty on $\log\epsilon$ (X) from Table 4; $\sigma _f$ : $\sigma _{\rm [X/Fe]}$ , the uncertainty on [Ru/Fe] or [Hf/Fe] from Table 4.
Table 6: Contributions of s- and r-processes for the abundances of Hf, Ru, Y, Eu, Sm, and Nd in solar system, following Arlandini et al. (1999). The last column is the sum of s- and r-processes.
Table 7: Least-square fits, [X₁/Fe] = A[X₂/Fe] + B, where X₁ is Ru or Hf and X₂ can be Y, Nd, Eu or Sm; "cov'' is the covariance between A and B; "d.o.f.'' is the number of degrees of freedom. Numbers in parenthesis are errors in last decimals.
Table 3: Equivalent width and abundance results for the sample stars, line by line. The symbol "<'' indicates an upper limit. The stars signaled with "*'' were considered normal rather than barium stars by Smiljanic et al. (2007).
Table 4: [Fe/H] and the mean values for $\log\epsilon$ (X) and [X/Fe] for all stars of the sample. The symbol "<'' indicates an upper limit. The stars signaled with "*'' were considered normal rather than barium stars by Smiljanic et al. (2007). The number of lines used to compute the medium is shown in brackets.
Table 5: This table was organized in increasing order of $T\rm _{eff}$ , with the comments about the results shown in the last column of each series of 4 columns.