... planets

Based on observations collected with the VLT/UT2 Kueyen telescope (Paranal Observatory, ESO, Chile) using the UVES spectrograph (Observing runs 66.C-0116 A and 66.D-0284 A), and with the William Herschel and Nordic Optical Telescopes, operated at the island of La Palma by the Isaac Newton Group and jointly by Denmark, Finland, Iceland, and Norway, respectively, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias.

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... systems)

Counts of January 2002. For a list see e.g. table at obswww.unige.ch/~naef/who_discovered_that_planet.html

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... present

Preliminary results were already presented in García López et al. (2001).

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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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... paper

The list of atmospheric parameters in Santos et al. (2001a) was determined by these authors for part of the objects, or was taken from the studies of Gonzalez (1998), Gonzalez & Laws (1998), and Gonzalez et al. (1999, 2001).

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... 0.15 dex

Note that these small uncertainties are relative, and not absolute.

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... factor

For this calculation we have used a Be/Fe ratio similar to C1 chondrites, and considered an iron content of $\sim$20% by mass (Anders & Grevesse 1989). Note also that the fall of a few jupiter-mass jovian planet(s) would not have a big effect on the iron or beryllium abundance of the star.

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...1990)

Improved Yale models (e.g. Deliyannis & Pinsonneault 1993) do not show an important difference. The 1990 models were thus used in the current paper, since they are the only tabulated.

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... models

We will assume for now that the initial Be abundance was similar (within the uncertainties) for all the stars in the plot.

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... trend

Can the presence of a massive proto-planetary disk (able to form planets), or other variables connected to the process of planetary formation itself (e.g. timescale), induce different angular momentum histories for stars with different $T_{\rm eff}$?

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