Context :

Aims : We use integrated-light spectroscopic observations to measure metallicities and chemical abundances for two extragalactic young massive star clusters ( NGC1313-379 and NGC1705-1 ) .
The spectra were obtained with the X-Shooter spectrograph on the ESO Very Large Telescope .

Methods : We compute synthetic integrated-light spectra , based on colour-magnitude diagrams for the brightest stars in the clusters from Hubble Space Telescope photometry and theoretical isochrones .
Furthermore , we test the uncertainties arising from the use of Colour Magnitude Diagram ( CMD ) +Isochrone method compared to an Isochrone-Only method .
The abundances of the model spectra are iteratively adjusted until the best fit to the observations is obtained .
In this work we mainly focus on the optical part of the spectra .

Results : We find metallicities of [ Fe/H ] = - 0.84 \pm 0.07 and [ Fe/H ] = - 0.78 \pm 0.10 for NGC1313-379 and NGC1705-1 , respectively .
We measure [ \alpha /Fe ] = + 0.06 \pm 0.11 for NGC1313-379 and a super-solar [ \alpha /Fe ] = + 0.32 \pm 0.12 for NGC1705-1 .
The roughly solar [ \alpha /Fe ] ratio in NGC1313-379 resembles those for young stellar populations in the Milky Way ( MW ) and the Magellanic Clouds , whereas the enhanced [ \alpha /Fe ] ratio in NGC1705-1 is similar to that found for the cluster NGC1569-B by previous studies .
Such super-solar [ \alpha /Fe ] ratios are also predicted by chemical evolution models that incorporate the bursty star formation histories of these dwarf galaxies .
Furthermore , our \alpha -element abundances agree with abundance measurements from H II regions in both galaxies .
In general we derive Fe-peak abundances similar to those observed in the MW and Large Magellanic Cloud ( LMC ) for both young massive clusters .
For these elements , however , we recommend higher-resolution observations to improve the Fe-peak abundance measurements .

Conclusions :