%0 Journal Article %T VLT/FLAMES high-resolution chemical abundances in Sculptor: a textbook dwarf spheroidal galaxy %A A. Helmi %A A. Kaufer %A B. Letarte %A E. Starkenburg %A E. Tolstoy %A F. Primas %A G. Battaglia %A K. A. Venn %A M. D. Shetrone %A M. Spite %A P. Fran£¿ois %A P. Jablonka %A T. J. L. de Boer %A V. Hill %A ¨¢. Sk¨²lad¨®ttir %J - %D 2019 %R 10.1051/0004-6361/201833950 %X We present detailed chemical abundances for 99 red-giant branch stars in the centre of the Sculptor dwarf spheroidal galaxy, which have been obtained from high-resolution VLT/FLAMES spectroscopy. The abundances of Li, Na, ¦Á-elements (O, Mg, Si, Ca Ti), iron-peak elements (Sc, Cr, Fe, Co, Ni, Zn), and r- and s-process elements (Ba, La, Nd, Eu) were all derived using stellar atmosphere models and semi-automated analysis techniques. The iron abundances populate the whole metallicity distribution of the galaxy with the exception of the very low metallicity tail, £¿2.3 ¡Ü [Fe/H] ¡Ü £¿0.9. There is a marked decrease in [¦Á/Fe] over our sample, from the Galactic halo plateau value at low [Fe/H] and then, after a ¡°knee¡±, a decrease to sub-solar [¦Á/Fe] at high [Fe/H]. This is consistent with products of core-collapse supernovae dominating at early times, followed by the onset of supernovae type Ia as early as ¡«12 Gyr ago. The s-process products from low-mass AGB stars also participate in the chemical evolution of Sculptor on a timescale comparable to that of supernovae type Ia. However, the r-process is consistent with having no time delay relative to core-collapse supernovae, at least at the later stages of the chemical evolution in Sculptor. Using the simple and well-behaved chemical evolution of Sculptor, we further derive empirical constraints on the relative importance of massive stars and supernovae type Ia to the nucleosynthesis of individual iron-peak and ¦Á-elements. The most important contribution of supernovae type Ia is to the iron-peak elements: Fe, Cr, and Mn. There is, however, also a modest but non-negligible contribution to both the heavier ¦Á-elements: S, Ca and Ti, and some of the iron-peak elements: Sc and Co. We see only a very small or no contribution to O, Mg, Ni, and Zn from supernovae type Ia in Sculptor. The observed chemical abundances in Sculptor show no evidence of a significantly different initial mass function, compared to that of the Milky Way. With the exception of neutron-capture elements at low [Fe/H], the scatter around mean trends in Sculptor for [Fe/H]£¿> £¿£¿2.3 is extremely low, and compatible with observational errors. Combined with the small scatter in the age-elemental abundances relation, this calls for an efficient mixing of metals in the gas in the centre of Sculptor since ¡«12 Gyr ago %U https://www.aanda.org/articles/aa/full_html/2019/06/aa33950-18/aa33950-18.html