Chemical abundances in a metal-poor RGB star

The results are based on equivalent width and spectrum synthesis analyses of a high-resolution (R~30000) 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 +17{deg}3248. 2MASS 18174532-3353235 also shares many chemical characteristics with the similar metallicity but comparatively {alpha}-poor Ursa Minor dwarf galaxy giant COS 82.