The Chemical Composition of Red Giant Stars in NGC4147

Details The Chemical Composition of Red Giant Stars in NGC4147 The Chemical Composition of Red Giant Stars in NGC4147

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21340716i&link_type=abstract

American Astronomical Society, AAS Meeting #213, #341.06; Bulletin of the American Astronomical Society, Vol. 41, p.205

Astronomy and Astrophysics

Astronomy

Scientific paper

According to recent literature, NGC4147 is a low-metallicity ([Fe/H] = -1.8) globular cluster associated with Sgr tidal stream, and is assumed to be a previous member of the Sgr dwarf galaxy. With little known about the chemical composition of metal-poor stars in Sgr, high signal-to-noise spectra were gathered of NGC4147 as a proxy indicator of the enrichment of Sgr at low metallicity. Detailed chemical compositions have been derived for four red giant stars. From Keck I HIRES data, [Fe/H] = -1.7 ± 0.1; [O/Fe] = 0.2 ± 0.2; [Na/Fe] = 0.2 ± 0.3; [Mg/Fe] = 0.45 ± 0.1; [Si/Fe] = 0.4 ± 0.15; [Ca/Fe] = 0.3 ± 0.05; [Zn/Fe] = 0.2 ± 0.1; [Ba,La/Fe] = 0.2 ± 0.1. These abundances, as well as an average combined [alpha/Fe] = 0.3, are all similar to that of the Milky Way field star population at this metallicity. We find none of the unusual abundances observed in Sgr field or globular cluster stars of higher metallicities. So, if NGC4147 is a proxy indicator of the stellar population of the Sgr dSph, then the nucleosynthetic history of Sgr up to this point seems to be shared with that of the Milky Way, and the divergence of their nucleosynthetic histories occcurs at a higher metallicity than [Fe/H] = -1.7.

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