Volume 385, Number 2, April II 2002
|Page(s)||L14 - L17|
|Published online||15 April 2002|
Letter to the Editor
Institute of Physics and Astronomy, Aarhus University, Ny Munkegade, 8000 Aarhus C, Denmark e-mail: fgj, firstname.lastname@example.org
2 University of Wisconsin Oshkosh, Oshkosh, WI 54901, USA e-mail: email@example.com
3 Lunds Observatory, Box 43, 221 00 Lund, Sweden e-mail: firstname.lastname@example.org
Corresponding author: F. Grundahl, email@example.com
Accepted: 17 February 2002
Abundances of O, Fe, Al, Mg, Na and Li determined from high-resolution and high signal–to–noise spectra of 21 red giant branch (RGB) stars in the globular cluster NGC 6752 are presented. We demonstrate that the Strömgren c1 index correlates extremely well with the measured NH, CH and CN indices and that variations in c1 are due to differences in UV NH band strengths. As shown by Grundahl et al. ([CITE]), the RGB stars in all 20 globular clusters surveyed possess large star-to-star variations in their c1 index, which we interpret as significant inhomogeneities in N abundances. The well known relations among O and Na and Mg and Al as well as with CN, CH, and NH are also present in these stars, some of which are fainter than the RGB bump. We find that the Li (6708 Å) equivalent width becomes too small to be measured as the luminosity of the stars increase above the luminosity of the RGB bump. Taken together, these data enforce the results of Gratton et al. ([CITE]) for turnoff and sub–giant branch stars, and suggest that in this cluster the abundance correlations observed among the brighter giants are in place prior to appreciable RGB ascent and likely due to previous generation(s) of stars, rather than due to mixing in the observed stars.
Key words: globular clusters / individual: NGC 6752 / stars: abundances / mixing
© ESO, 2002
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