Chemistry of Messier 31

Details Chemistry of Messier 31 Chemistry of Messier 31

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8745w&link_type=abstract

HST Proposal ID #8745

Computer Science

Hst Proposal Id #8745 Stellar Populations

Scientific paper

Sampling local group spiral M31 from its nucleus to regions where its halo fades to nothing, stellar color-magnitude diagrams of the brighter giants will be used to construct histograms of {fraction of stars} as a function of {abundance} at each radial location. From these abundance distributions the following will be derived: {1} the overall radial abundance gradient in the disk and spheroid of M31 from stars, not nebulae, and {2} the simulated all-M31 ``closed box'' abundance distribution. These data will be far more complete and homogeneous than data available for the Milky Way. Chemical evolution models will be applied to the data. If the observed paucity of metal-poor stars in the outer disk of M31 continues to the M31 outskirts, it will be impossible to reconcile any constant-yield model with the M31 data, and, by inference, spirals in general.

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