High Resolution Spectroscopy of Metal-Rich Halo Stars

Details High Resolution Spectroscopy of Metal-Rich Halo Stars High Resolution Spectroscopy of Metal-Rich Halo Stars

Apr 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aspc...92..351b&link_type=abstract

Formation of the Galactic Halo...Inside and Out, ASP Conference Series, Vol. 92, 1996, Heather Morrison and Ata Sarajedini, eds.

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Scientific paper

We have used high resolution spectroscopy to test the claim of a high metallicity population in an in situ population of the galactic halo. High resolution spectra (R = 30,000) were taken of our giant star candidates over the wavelength range of 4880 - 6880 Angstroms, with which classical line abundance analyses were performed to deduce abundances. Iron abundances indicate that [m/H] values derived through metallicity indices are correct for [Fe/H] >= --0.5, but that many supposed metal-rich stars with [Fe/H] <= --0.5 are actually much more metal-poor than DDO photometry would indicate. For truly metal-rich stars, abundances of other heavy elements relative to iron conform to well defined halo abundance patterns. Neither inhomogeneous chemical evolution of the halo nor mergers of satellite galaxies can be ruled out by these abundances.

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