... 6752[*]
Based on observations collected at ESO telescopes under programme 073.D-0211. 
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...[*]
Full Tables 2, 3 and 5 are only available in electronic form 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/464/927 
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... metallicity[*]
We adopt the usual spectroscopic notation, i.e. [X] = log (X) $_{\rm star} -$ log (X)$_\odot$ for any abundance quantity X, and log $\epsilon$(X) = log (NX/$N_{\rm H}$) + 12.0 for absolute number density abundances. 
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... IRAF[*]
IRAF is distributed by the National Optical Astronomical Observatory, which are operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. 
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...Å[*]
The analysis of UVES spectra in NGC 6752 as well as in the other globular clusters studied in the present project will be presented separately. 
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... UVES spectra[*]
The difference between the UVES and GIRAFFE EWs we found for NGC 6752 spectra is larger than observed for other GCs analyzed in this series. This difference is not simply a function of metallicity. Inspection of the original spectra showed that this difference is not due to the measuring procedure and that lines in spectra of stars at the same position in the CMD may be of different strength. We think that this is due to small but significant effects intrinsic to the GIRAFFE spectra. Our procedure reduces to a minimum the systematic error for each GC. 
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...%[*]
EWs measured on moderate resolution spectra may be either overestimated due to contribution of blends, not recognized when compiling the line list, or underestimated, because the nominal continuum used when extracting EWs can be lower than the real value, due to veiling from weak lines, not recognized as such due to the low resolution of the spectrum. 
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... -1.42[*]
This value is somewhat different from what we derive in the present study (i.e. -1.56), but the dependence of (V-K) on [Fe/H] is so weak that temperatures are unaffected. 
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...$\sigma$ value[*]
This value was derived as the quadratic mean of the 1$\sigma$ errors in the slope of the relation between abundance and expected line strength for all stars with more than 15 lines measured. 
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... AGB stars[*]
Very recently, Prantzos & Charbonnel (2006) suggested instead that the Na-O anticorrelation is due to nucleosynthesis in rapidly rotating massive stars rather than in AGB stars. While this difference would not affect most of the present discussion, we note that the very small scatter in Fe abundances sets stringent limits on the "inefficiency'' of mixing between the slow winds of stars in the supergiant phases and the ejecta from core-collapse supernovae in this scenario. 
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Copyright ESO 2007