Elemental Abundance Ratios in Stars of the Outer Galactic Disk. I. Open Clusters

Details Elemental Abundance Ratios in Stars of the Outer Galactic Disk. I. Open Clusters Elemental Abundance Ratios in Stars of the Outer Galactic Disk. I. Open Clusters

2005-04-07

arxiv.org/abs/astro-ph/0504193v1

Astron.J.130:597-625,2005

Astronomy and Astrophysics

Astrophysics

Accepted for publication in AJ

Scientific paper

10.1086/430934

We summarize radial velocity studies of selected stars in the old, distant clusters Berkeley 20, Berkeley 21, NGC 2141, Berkeley 29, and Berkeley 31. Three members of M67 were observed similarly, and those velocities compare extremely well with prior measures. We measured the chemical compositions of all six clusters for [Fe/H] as well as abundances of alpha elements, iron-peak elements, and those synthesized in either the s-process or the r-process. For the outer disk, the abundance gradient for [Fe/H] deviates from the trend defined near the solar neighborhood. Rather than declining with increasing Galactocentric distance, [Fe/H] appears to reach a "basement" at [Fe/H]=-0.5 beyond R_GC = 10 to 12kpc. We find enhanced [O/Fe], [alpha/Fe], and [Eu/Fe] in the outer disk revealing a rapid star formation history. An intriguing, but tentative, conclusion is that the outer disk open cluster abundance ratios are consistent with the outer disk being formed via a merger event. The basement in [Fe/H] and enhanced [alpha/Fe] suggest that the outer disk formed from a reservoir of gas with a star formation history distinct from the solar neighborhood. The open clusters may have formed as a result of star formation triggered by a merger event in the outer disk. The ages of the outer disk open clusters would then be a measure of when the merger occurred. [Abridged]

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