Recent studies show that rotation significantly affects the s-process in massive stars. We provide tables of yields for non-rotating and rotating massive stars between 10 and 150 $M_{odot}$ at $Z=10^{-3}$ ([Fe/H] $=-1.8$). Tables for different mass cuts are provided. The complete s-process is followed during the whole evolution with a network of 737 isotopes, from Hydrogen to Polonium. A grid of stellar models with initial masses of 10, 15, 20, 25, 40, 60, 85, 120 and 150 $M_{odot}$ and with an initial rotation rate of both 0 or 40$~%$ of the critical velocity was computed. Three extra models were computed in order to investigate the effect of faster rotation (70$~%$ of the critical velocity) and of a lower $^{17}$O($alpha,gamma$) reaction rate. At the considered metallicity, rotation has a strong impact on the production of s-elements for initial masses between 20 and 60 $M_{odot}$. In this range, the first s-process peak is boosted by $2-3$ dex if rotation is included. Above 60 $M_{odot}$, s-element yields of rotating and non-rotating models are similar. Increasing the initial rotation from 40$~%$ to 70$~%$ of the critical velocity enhances the production of $40 lesssim Z lesssim 60$ elements by $sim 0.5-1$ dex. Adopting a reasonably lower $^{17}$O($alpha,gamma$) rate in the fast rotating model (70$~%$ of the critical velocity) boosts again the yields of s-elements with $55 lesssim Z lesssim 82$ by about 1 dex. In particular, a modest amount of Pb is produced. Together with s-elements, some light elements (particularly fluorine) are strongly overproduced in rotating models.
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