... exoplanets

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.

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... planets

See e.g. tables at http://obswww.unige.ch/exoplanets/

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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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... (see Paper II)

These represent relative errors, and not absolute ones.

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... high

In this case the estimated errors in $T_{{\rm eff}}$, $\log{g}$, $\xi _t$ and [Fe/H] are of 150 K, 0.40 dex, 0.15 km s^-1, and 0.17 dex, respectively.

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...

The only star not used was HD137759 (a K giant); we prefer to keep it out in the rest of the analysis.

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... determination

These are: GJ 876 (an M dwarf), HD 40979, HD 49674, HD 68988, HD 72659, HD 73526, and HD 76700.

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... sample

These are: HD 142, HD 1237, HD 4208, HD 6434, HD 13445, HD 16141, HD 17051, HD 19994, HD 22049, HD 23079, HD 28185, HD 39091, HD 52265, HD 75289, HD 82943, HD 83443, HD 92788, HD 108147, HD 114386, HD 114729, HD 114783, HD 121504, HD 130322, HD 134987, HD 141937, HD 147513, HD 160691, HD 162020, HD 168443, HD 168746, HD 169830, HD 179949, HD 192263, HD 196050, HD 202206, HD 210277, HD 213240, HD 216435, HD 216437, HD 217107, and HD 222582.

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... error

This value has only recently been improved to about 2-3 m s^-1 (Queloz et al. 2001; Pepe et al. 2002).

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... readily

To our knowledge, there is no study to date of the variations in the mass of proto-planetary disks as a function of stellar mass for solar-type stars.

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... mass

This quantity was derived using the equations presented in Murray et al. (2001).

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... material

A 1 $M_{\odot}$ solar metallicity star reaches the main-sequence after $\sim$30 Myr.

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... excess

These facts can even be seen as a constraint for the timescales of disk evolution and giant planet formation.

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...$M_{{\rm Jup}}$

As shown by Jorissen et al. (2001), this is a probable upper limit for the mass of a planet.

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... planet

The higher the dust density of the disk, the bigger will be the core mass you might be able to form (e.g. Kokubo & Ida 2002); does this mass influence the final mass of the giant planet?

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... "short''

With short we refer here to planets having periods that are, in average, shorter than the ones found around more metal-rich stars.

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... velocities

U, V and W represent the usual spatial velocities of a star in the direction of the the galactic center, galactic rotation, and perpendicular to the galactic plane, respectively.

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...1997)

The values of U, V and W for the planet host stars will be available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/398/363

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