... stars[*]
Based on observations collected at the La Silla Observatory, ESO (Chile), with the CORALIE spectrograph at the 1.2-m Euler Swiss telescope and the FEROS spectrograph at the 1.52-m ESO telescope, with the VLT/UT2 Kueyen telescope (Paranal Observatory, ESO, Chile) using the UVES spectrograph (Observing run 67.C-0206, in service mode), with the TNG and William Herschel Telescopes, both operated at the island of La Palma, and with the ELODIE spectrograph at the 1.93-m telescope at the Observatoire de Haute Provence.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... case[*]
With probably the only exception being the studies of beryllium by Santos et al. (2002).
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... IRAF[*]
IRAF is distributed by National Optical Astronomy Observatories, operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation, USA.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... [Fe/H])[*]
The usual errors in this quantity for the stars in our sample are smaller than this value (Santos et al. 2001).
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... 0.10 dex[*]
In a relative and not absolute sense.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... Appendix[*]
These 4 elements seem to suffer the strongest NLTE effects; furthermore, in average, planet hosts have higher $T_{\rm eff}$ than stars without planets by about 250 K.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... subject[*]
This comparison might be seen (also) as a test for the reliability of our analysis.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... plots[*]
But as noted in the last section, there are no discontinuities between the two samples.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
... sample[*]
We stress that this trend is only slightly significant for this metallicity regime. Stars with [Fe/H] between -0.1 and 0.1 have, for example, the "same'' average $T_{\rm eff}$ as the objects with [Fe/H] above 0.3.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
...$T_{\rm eff}$[*]
We have done plots of the [Fe/H] abundances as a function of $T_{\rm eff}$, $\log{g}$, and $\xi_{\rm t}$, and have found no significant trends. This gives us confidence about the reliability of our analysis, as expected since for solar-metallicity stars neither Fe I or Fe II (on which our parameter analysis relied, Santos et al. 2000) do not seem to suffer from "important'' NLTE effects.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
.
Copyright ESO 2003