Possible Identification of a Metal-Rich Old Moving Group: High-Resolution Spectroscopy of Candidate Members

Details Possible Identification of a Metal-Rich Old Moving Group: High-Resolution Spectroscopy of Candidate Members Possible Identification of a Metal-Rich Old Moving Group: High-Resolution Spectroscopy of Candidate Members

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aj....133.2654d&link_type=abstract

The Astronomical Journal, Volume 133, Issue 6, pp. 2654-2658.

Astronomy and Astrophysics

Astronomy

Open Clusters And Associations: General, Stars: Abundances, Stars: Evolution, Stars: Late-Type

Scientific paper

Using new high-resolution spectroscopic observations from both the McDonald Observatory 2.7 m and Kitt Peak National Observatory 4 m telescopes, we observed four candidate members of the Ursa Major moving group previously suggested to instead belong to a significantly older kinematic assemblage. The Fe abundances we measure strongly suggest that these stars are not UMa members but form a more metal-rich group of stars (+0.10<=[Fe/H]<=+0.18) with an age near 3 Gyr. Our [Ca/H] determinations corroborate this result. The apparent similarities in metallicity and previously discovered UVW space motions lend credence to prior suggestions that these stars belong to a field kinematic structure of uniform age. Li abundances have also been derived from the 6707 Å feature for all four stars and show the differences expected from the stars' varying evolutionary states. The low Li abundance of one object, HD 88654, does not support its previously reported status as a post-T Tauri star candidate.
This paper includes data taken at the McDonald Observatory of the University of Texas at Austin.
Based on observations obtained at Kitt Peak National Observatory, a division of the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.

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