Based on observations collected at the La Silla Observatory, ESO (Chile), with the CORALIE spectrograph at the 1.2-m Euler Swiss telescope, with the FEROS spectrograph at the 1.52-m ESO telescope (Observing run 66.C-0116 B), and using the UES spectrograph at the 4-m William Hershel Telescope (WHT), at La Palma (Canary Islands).

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Here we are referring to the known extrasolar planetary host stars, having Jupiter-like planets in relatively short period orbits when compared to the giant planets in our own Solar System.

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... 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.

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... spectroscopy

The errors in mass represent simply formal errors, computed using the uncertainties in $T_{\rm eff}$ and M_V.

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... sample

These include HD 1237, HD 6434, HD 13445, HD 16141, HD 17051, HD 19994, HD 22049, HD 28185, HD 52265, HD 75289, HD 82943, HD 83443, HD 92788, HD 108147, HD 121504, HD 130322, HD 134987, HD 168443, HD 168746, HD 169830, HD 192263, HD 210277, HD 217107 and HD 222582.

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... preparation)

The cross-correlation dip can be seen as an average spectral line; as shown by Mayor (1980) and Pont (1997) its surface is well correlated with [Fe/H] and (B-V). A calibration of its surface with these two variables can in fact be used to obtain in a very simple way precise metallicity estimates, at least in a statistical sense. In this particular case, the calibration used to construct this "comparison'' sample uses as "calibrators'' the stars presented in Tables 1 and 2, and thus the results are in the same [Fe/H] scale as our spectroscopic values. The precision of the calibration is remarkable ( ${\rm rms}\sim0.01$ dex). The resulting distribution is quite symmetric, and peeks at $\sim$ -0.05 dex.

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