All Figures

Figure 1: Metallicity distribution for 119 planet-host stars (dashed line) and for a volume-limited "comparison'' sample of 94 stars with no known planetary-mass companions (continuous line). The metallicities were taken from Table 1, Table 2 and from Tables 2-5 of Santos et al. (2004b). The difference between the average metallicity of two samples is 0.24 dex. Inset: cumulative functions for both distributions. A Kolmogorov-Smirnov test shows that the probability that both distributions belong to the same population is of the order of 10-12.

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In the text

Figure 2: Metallicity distribution for 22 planet-host stars in binary stellar systems (PIB - filled line) when compared with the same distribution for single planet-hosts (dashed line). The metallicities were taken from Table 1 and from Santos et al. (2004b). The difference between the average metallicity of two samples is 0.03 dex, PIB stars being slighly overabundant. Inset: cumulative functions for both distributions. A Kolmogorov-Smirnov test shows that the probability that both distributions belong to the same population is of the order of 0.08.

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In the text