We have constructed the 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 \textrm { [ Fe / H ] } \leq - 2.5 , and more than 6000 stars in the local group galaxies .
We examined a validity of using a combined data set for elemental abundances .
We also checked a consistency between the derived distances to individual stars and those to galaxies in the literature values .
Using the updated database , the characteristics of stars in dwarf galaxies are discussed .
Our statistical analyses of \alpha -element abundances show that the change of the slope of the [ \alpha /Fe ] relative to [ Fe/H ] ( so-called “ knee ” ) occurs at \textrm { [ Fe / H ] } = -1.0 \pm 0.1 for the Milky Way .
The knee positions for selected galaxies are derived by applying the same method .
Star formation history of individual galaxies are 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 \textrm { [ Fe / H ] } \lesssim - 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 characterises the abundance trends in the Galactic globular clusters .