A high-resolution VLT/FLAMES study of individual stars in the centre of the Fornax dwarf spheroidal galaxy
For the first time we show the detailed, late-stage, chemical evolution history of a small nearby dwarf spheroidal galaxy in the Local 
Group. We present the results of a high-resolution (R ~ 20 000, λ = 5340–5620; 6120–6701) FLAMES/GIRAFFE abundance study 
at ESO/VLT of 81 photometrically selected, red giant branch stars in the central 25 of the Fornax dwarf spheroidal galaxy. We also 
carried out a detailed comparison of the effects of recent developments in abundance analysis (e.g., spherical models vs. plane-parallel) 
and the automation that is required to efficiently deal with such large data sets. We present abundances of α-elements (Mg, Si, Ca, 
and Ti), iron-peak elements (Fe, Ni, and Cr), and heavy elements (Y, Ba, La, Nd, and Eu). Our sample was randomly selected and 
is clearly dominated by the younger and more metal-rich component of Fornax, which represents the major fraction of stars in the 
central region. This means that the majority of our stars are 1−4 Gyr old, and thus represent the end phase of chemical evolution in 
this system. Our sample of stars has unusually low [α/Fe], [Ni/Fe], and [Na/Fe] compared to the Milky Way stellar populations at the 
same [Fe/H]. The particularly important role of stellar winds from low-metallicity AGB stars in the creation of s-process elements is 
clearly seen from the high [Ba/Y]. Furthermore, we present evidence of an s-process origin of Eu.