All Tables

Table 1: Atomic parameters of the spectral lines used for every element. Column 1: wavelength (in Å); Col. 2: excitation energy of the lower energy level in the transition (in eV); Col. 3: oscillator strengths based on an inverse solar analysis.
Table 2: Spectrographs and data characteristics.
Table 3: Slopes of [X/Fe] ratios as functions of effective temperatures per 1000 K (in dex) for both samples (planet hosts and non-hosts).
Table 4: Sensitivity of the abundances of Si, Ca, Sc, Ti, V, Cr, Mn, Co and Ni to changes of 100 K in $T_{\rm eff}$ , 0.30 dex in $\log g$ and [Fe/H], 0.50 km s^-1 in $\xi _{\rm t}$ .
Table 5: The same as Table 4 but for Na, Mg and Al.
Table 6: Average abundances $\langle[X$ /H $]\rangle$ for stars with planets and for comparison sample stars. For each element the rms around the mean and the abundances difference between the two samples (101 and 93 respectively) are also listed.
Table 7: Stars with giant planets and abundances derived for Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni.
Table 8: Stars without giant planets and abundances derived for Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni.
Table 9: Abundances of Na, Mg and Al (from Beirão et al. 2005, with the addition of our results) and atmospheric parameters (from Santos et al. 2004b, 2005) for stars with planets.
Table 10: Abundances of Na, Mg and Al (from Beirão et al. 2005, with the addition of our results) and atmospheric parameters (from Santos et al. 2004b, 2005) for stars without planets.