Giant Star Metallicities from Low-Signal-to-Noise Spectra

Details Giant Star Metallicities from Low-Signal-to-Noise Spectra Giant Star Metallicities from Low-Signal-to-Noise Spectra

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.2602l&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #26.02; Bulletin of the American Astronomical Society, Vol. 24, p.767

Astronomy and Astrophysics

Astronomy

Scientific paper

Low-signal-to-noise spectra have now been used very successfully to obtain accurate metal abundances for large numbers of field dwarf stars (Laird, Carney, and Latham 1988) using least squares comparison to a grid of synthetic spectra. The extension of this technique to giant stars would provide the means to study much more distant objects, including the LMC. As a prelude to work on LMC field giants, we have obtained echelle spectra using Argus at CTIO of giants in a number of Milky Way clusters to investigate further the low-S/N technique. We will present the results and compare them to those of higher S/N, lower resolution methods.

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