Stellar Abundances for Galactic Archaeology Database. IV. Compilation of stars in dwarf galaxies

• Published in: Publications of the Astronomical Society of Japan Vol. 69; no. 5
• Main Authors: Suda, Takuma, Hidaka, Jun, Aoki, Wako, Katsuta, Yutaka, Yamada, Shimako, Fujimoto, Masayuki Y., Ohtani, Yukari, Masuyama, Miyu, Noda, Kazuhiro, Wada, Kentaro
• Format: Journal Article
• Language: English
• Published: Oxford University Press 01.10.2017
• Subjects: stars: evolution; astronomical data bases: miscellaneous; stars: abundances
• ISSN: 0004-6264; 2053-051X
• DOI: 10.1093/pasj/psx059

Abstract We have constructed a database of stars in Local Group galaxies using the extended version of the SAGA (Stellar Abundances for Galactic Archaeology) database that contains stars in 24 dwarf spheroidal galaxies and ultra-faint dwarfs. The new version of the database includes more than 4500 stars in the Milky Way, by removing the previous metallicity criterion of [Fe/H] ≤ −2.5, and more than 6000 stars in the Local Group galaxies. We examined the validity of using a combined data set for elemental abundances. We also checked the consistency between the derived distances to individual stars and those to galaxies as given in the literature. Using the updated database, the characteristics of stars in dwarf galaxies are discussed. Our statistical analyses of α-element abundances show that the change of the slope of the [α/Fe] relative to [Fe/H] (so-called “knee”) occurs at [Fe/H] = −1.0 ± 0.1 for the Milky Way. The knee positions for selected galaxies are derived by applying the same method. The star formation history of individual galaxies is explored using the slope of the cumulative metallicity distribution function. Radial gradients along the four directions are inspected in six galaxies where we find no direction-dependence of metallicity gradients along the major and minor axes. The compilation of all the available data shows a lack of CEMP-s population in dwarf galaxies, while there may be some CEMP-no stars at [Fe/H] ≲ −3 even in the very small sample. The inspection of the relationship between Eu and Ba abundances confirms an anomalously Ba-rich population in Fornax, which indicates a pre-enrichment of interstellar gas with r-process elements. We do not find any evidence of anti-correlations in O–Na and Mg–Al abundances, which characterizes the abundance trends in the Galactic globular clusters.