The chemical evolution of the Bootes I ultra-faint dwarf galaxy

We present chemical abundance measurements of two metal-poor red giant stars in the ultra-faint dwarf galaxy Boötes I, based on Magellan/MIKE high-resolution spectra. For Boo-980, with [Fe/H] = -3.1, we present the first elemental abundance measurements, while Boo-127, with [Fe/H] = -2.0, shows abundances in good agreement with previous measurements. Light and iron-peak element abundance ratios in the two Boötes I stars, as well as those of most other Boötes I members, collected from the literature, closely resemble those of regular metal-poor halo stars. Neutron-capture element abundances Sr and Ba are systematically lower than the main halo trend and also show a significant abundance spread. Overall, this is similar to what has been found for other ultrafaint dwarf galaxies. We apply corrections to the carbon abundances (commensurate with stellar evolutionary status) of the entire sample and find 21% of stars to be carbon-enhanced metal-poor (CEMP) stars, compared to 13% without using the carbon correction. We reassess the metallicity distribution functions for the CEMP stars and non-CEMP stars, and confirm earlier claims that CEMP stars might belong to a different, earlier population. Applying a set of abundance criteria to test to what extent Boötes I could be a surviving first galaxy suggests that it is one of the earliest assembled systems that perhaps received gas from accretion from other clouds in the system, or from swallowing a first galaxy or building block type object. This resulted in the two stellar populations observable today.A.F. is supported by NSF CAREER grant AST-1255160. She also acknowledges support from the Silverman (1968) Family Career Development Professorship. Studies at RSAA, ANU, of the Galaxy’s most metal-poor stars and ultra-faint satellite systems are supported by Australian Research Council grants DP0663562, DP0984924, DP120100475, and DP150100862 which J.E.N. gratefully acknowledges