On the question of a metallicity spread in globular cluster M22 (NGC 6656)

Details On the question of a metallicity spread in globular cluster M22 (NGC 6656) On the question of a metallicity spread in globular cluster M22 (NGC 6656)

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005hia....13..150i&link_type=abstract

In: Highlights of Astronomy, Vol. 13, as presented at the XXVth General Assembly of the IAU - 2003 [Sydney, Australia, 13 - 26 J

Astronomy and Astrophysics

Astronomy

Globular Clusters, Element Abundances

Scientific paper

Results from early photometric and spectroscopic studies found that M22 (NGC 6656) showed a metallicity spread similar to albeit significantly smaller than that found in Omega Cen the most massive cluster in our Galaxy. Numerous investigations of M22 have been made which have yielded conflicting results. Depending upon the sample and analysis techniques some studies report no significant variations whereas others have found metallicity variations on the order of half a dex.
In this new investigation we employ high resolution high signal-to-noise spectra and a variety of spectroscopic approaches in determining the metallicity of a sample of 30 stars in M22. Results of experiments with an ensemble of models with a range of Teffs and loggs allows us to plot a region in the Teff/[Fe/H] and logg/[Fe/H] plane for each star. Examination of preliminary results for 5 stars shows a narrow region of 0.05 dex in the [Fe/H] parameter that satisfies all of the stars done thus far. This method also allows us to explore how the previously reported metallicity spreads may have been obtained.

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