The chemical compositions of 26 distant late-type supergiants and the metallicity gradient in the galactic disk

Details The chemical compositions of 26 distant late-type supergiants and the metallicity gradient in the galactic disk The chemical compositions of 26 distant late-type supergiants and the metallicity gradient in the galactic disk

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...241..218l&link_type=abstract

Astrophysical Journal, Part 1, vol. 241, Oct. 1, 1980, p. 218-228.

Astronomy and Astrophysics

Astrophysics

36

Abundance, Chemical Composition, Galactic Structure, Late Stars, Milky Way Galaxy, Supergiant Stars, Spectral Line Width, Tables (Data)

Scientific paper

From an analysis of high-dispersion Mount Wilson spectroscopic data, we have obtained atmospheric parameters and chemical abundances for 26 distant supergiants of spectral types G through M. Iron-to-hydrogen ratios with respect to the Sun, [Fe/H], can be determined from this material with an uncertainty of ±0.2 dex.
It is found that supergiants more than about 0.5 kpc from the Sun in the direction of the galactic anticenter are significantly metal-deficient relative to those in the solar neighborhood. Combining our new analyses with those published earlier by Luck for 28 additional supergiants, we derive a radial metallicity gradient d[Fe/H]/dR = -0.24 ± 0.04 kpc-1 for the region of the galactic disk between 7.7 and 10.2 kpc from the galactic center. This gradient is steeper than is found from older objects (such as field main-sequence stars, red giants, and open clusters) and suggests that the metallicity gradients in disk galaxies steepen significantly with age.

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