All Figures

	Figure 1: UVES spectra of the two turn-off stars 200613 and 4428 of the GC NGC 6752. The dotted lines correspond to the Be abundances (upper limit) for star 200613 and for star 4428.
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In the text

	Figure 2: UVES spectra of stars 200613 and 4428 around the NH band at 336 nm. The band is much stronger in star 200613, indicating a strong N overabundance. Solid lines are the observed spectra; thin lines are synthetic spectra computed with parameters appropriate to the program stars, and N abundances of [N/Fe] = 0, 0.4, 0.8, 1.2, 1.6 and 2.0.
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In the text

Figure 3: Evolution of Be with time in the Galaxy according to a three-zone Galactic chemical evolution model (Valle et al. 2002). The three curves refer to the halo, thick disk, and thin disk. The data points show the Be abundance in the young open cluster IC 2391 (age 55 Myr), the Sun (age 4.5 Gyr), the globular clusters NGC 6397 (isochrone age  Gyr) and NGC 6752 (isochrone age  Gyr). The model result is normalized to the solar meteoritic abundance. The inset shows a detail of the early Galactic evolution. The Be abundance of IC 2391 is from Randich et al. (2002); the Be abundances of the two GCs are from Pasquini et al. (2004) for NGC 6397 and from this work for NGC 6752. The isochrone ages are from Gratton et al. (2003).

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In the text

	Figure 4: Be abundance vs. Fe for the NGC 6397 ( filled circles) and the NGC 6752 TO star ( filled square) and the star from B99 ( open circles). The stars in the clusters are indistinguishable from the field stars.
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In the text

	Figure 5: Be abundance vs. O for the NGC 6397 ( filled circles) and the NGC 6752 TO stars ( filled square) and the star from B99 ( open circles). The "unpolluted'', O-rich stars in the clusters closely follow the field stars.
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In the text