  We report on a strictly differential line-by-line analysis of high quality
UVES spectra of bright giants in the metal-poor globular cluster NGC 6752. We
achieved high precision differential chemical abundance measurements for Fe,
Na, Si, Ca, Ti, Cr, Ni, Zn, Y, Zr, Ba, La, Ce, Pr, Nd, Sm, Eu and Dy with
uncertainties as low as ~0.01 dex (~2%). We obtained the following main
results. (1) The observed abundance dispersions are a factor of ~2 larger than
the average measurement uncertainty. (2) There are positive correlations, of
high statistical significance, between all elements and Na. (3) For any pair of
elements, there are positive correlations of high statistical significance,
although the amplitudes of the abundance variations are small. Removing
abundance trends with effective temperature and/or using a different pair of
reference stars does not alter these results. These abundance variations and
correlations may reflect a combination of (a) He abundance variations and (b)
inhomogeneous chemical evolution in the pre- or proto-cluster environment.
Regarding the former, the current constraints on Delta Y from photometry likely
preclude He as being the sole explanation. Regarding the latter, the
nucleosynthetic source(s) must have synthesised Na, alpha, Fe-peak and
neutron-capture elements and in constant amounts for species heavier than Si;
no individual object can achieve such nucleosynthesis. We speculate that other,
if not all, globular clusters may exhibit comparable abundance variations and
correlations to NGC 6752 if subjected to a similarly precise analysis.
