Chemical Abundances of three Metal-Poor Globular Clusters (NGC 6287, NGC 6293 and NGC 6541) in the Inner Halo

Details Chemical Abundances of three Metal-Poor Globular Clusters (NGC 6287, NGC 6293 and NGC 6541) in the Inner Halo Chemical Abundances of three Metal-Poor Globular Clusters (NGC 6287, NGC 6293 and NGC 6541) in the Inner Halo

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...199.5619l&link_type=abstract

American Astronomical Society, 199th AAS Meeting, #56.19; Bulletin of the American Astronomical Society, Vol. 33, p.1387

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Scientific paper

We present a chemical abundance study of the old inner halo clusters NGC 6287, NGC 6293, and NGC 6541. Our metallicity estimates for NGC 6287, NGC 6293, and NGC 6541 are [Fe/H] = -2.00 +/- 0.05, -2.01 +/- 0.02, and -1.78 +/- 0.02, respectively, and our metallicity measurements are in good agreement with previous estimates. The mean α -element abundances of our program clusters are in good agreement with other globular clusters, confirming previous results. However, the individual α -elements appear to follow different trends. The silicon abundances of the inner halo clusters appear to be enhanced and the titanium abundances appear to be depleted compared to the intermediate halo clusters. In particular, [Si/Ti] ratios appear to be related to the metallicities or Galactocentric distances, in the sense that [Si/Ti] ratios decrease with metallicity and Galactocentric distance. We propose that these [Si/Ti] gradients with metallicity or Galactocentric distance may be due to the different masses of the SNe II progenitors. The high [Si/Ti] ratios toward the Galactic center and at lower metallicities may be due to high-mass SNe II contributions.

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