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Neutron-capture elements, those with Z > 35, are the least well-understood interms of nucleosynthesis and formation environments. The rapid neutron-capture,or r-process, elements are formed in the environments and/or remnants ofmassive stars, while the slow neutron-capture, or s-process, elements areprimarily formed in low-mass AGB stars. These elements can provide muchinformation about Galactic star formation and enrichment, but observationaldata is limited. We have assembled a sample of 68 stars in 23 open clustersthat we use to probe abundance trends for six neutron-capture elements (Eu, Gd,Dy, Mo, Pr, and Nd) with cluster age and location in the disk of the Galaxy. Inorder to keep our analysis as homogenous as possible, we use an automatedsynthesis fitting program, which also enables us to measure multiple (3-10)lines for each element. We find that the pure r-process elements (Eu, Gd, andDy) have positive trends with increasing cluster age, while the mixed r- and s-process elements (Mo, Pr, and Nd) have insignificant trends consistent withzero. Pr, Nd, Eu, Gd, and Dy have similar, slight (though mostly statisticallysignificant) gradients of ~0.04 dex/kpc. The mixed elements also appear to havenonlinear relationships with Galactocentric radius.

New Neutron-Capture Measurements in 23 Open Clusters. I. The R-Process