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CHEMICAL ABUNDANCE ANALYSIS OF A NEUTRON-CAPTURE ENHANCED RED GIANT IN THE BULGE PLAUT FIELD

We present chemical abundances for 27 elements ranging from oxygen to erbium in the metal-poor ([Fe/H] = −1.67) bulge red giant branch star 2MASS 18174532–3353235. The results are based on equivalent width and spectrum synthesis analyses of a high-resolution (R ∼ 30, 000) spectrum obtained with the Magellan-MIKE spectrograph. While the light (Z ≲ 30) element abundance patterns match those of similar metallicity bulge and halo stars, the strongly enhanced heavy element abundances are more similar to “r-II” halo stars (e.g., CS 22892–052) typically found at [Fe/H] ≲ − 2.5. We find that the heaviest elements (Z ⩾ 56) closely follow the scaled-solar r-process abundance pattern. We do not find evidence supporting significant s-process contributions; however, the intermediate mass elements (e.g., Y and Zr) appear to have been produced through a different process than the heaviest elements. The light and heavy element abundance patterns of 2MASS 18174532–3353235 are in good agreement with the more metal-poor r-process enhanced stars CS 22892–052 and BD +17o3248. 2MASS 18174532–3353235 also shares many chemical characteristics with the similar metallicity but comparatively α-poor Ursa Minor dwarf galaxy giant COS 82. Interestingly, the Mo and Ru abundances of 2MASS 18174532–3353235 are also strongly enhanced and follow a similar trend recently found to be common in moderately metal-poor main-sequence turn-off halo stars.