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We present stellar parameters and metallicities, obtained from a detailedspectroscopic analysis, for a large sample of 98 stars known to be orbited byplanetary mass companions (almost all known targets), as well as for avolume-limited sample of 41 stars not known to host any planet. For most of thestars the stellar parameters are revised versions of the ones presented in ourprevious works. However, we also present parameters for 18 stars with planetsnot previously published, and a compilation of stellar parameters for theremaining 4 planet-hosts for which we could not obtain a spectrum. A comparisonof our stellar parameters with values of Teff, log(g), and [Fe/H] available inthe literature shows a remarkable agreement. The derived [Fe/H] values are thenused to confirm the previously known result that planets are more prevalentaround metal-rich stars. Furthermore, we confirm that the frequency of planetsis a strongly rising function of the stellar metallicity, at least for starswith [Fe/H]>0. While only about 3% of the solar metallicity stars in theCORALIE planet search sample were found to be orbited by a planet, this numberincreases to more than 25% for stars with [Fe/H] above +0.3. Curiously, ourresults also suggest that these percentages might remain relatively constantfor values of [Fe/H] lower than about solar, increasing then linearly with themass fraction of heavy elements. These results are discussed in the context ofthe theories of planetary formation.Comment: 15 pages, 9 figures, Accepted for publication in A&A; Replaced after  language editin

Spectroscopic [Fe/H] for 98 extra-solar planet-host stars