Context : Open clusters exquisitely track the Galactic disc chemical properties and its time evolution ; a substantial number of studies and large spectroscopic surveys focus mostly on the chemical content of relatively old clusters ( age \gtrsim 1 Gyr ) .
Interestingly , the less studied young counterpart populating the solar surrounding has been found to be solar ( at most ) , with a notable surprising lack of young metal-rich objects .
While there is wide consensus about the moderately above-solar composition of the Hyades cluster , the metallicity of Praesepe is still controversial .
Recent studies suggest that these two clusters share identical chemical composition and age , but this conclusion is disputed .

Aims : With the aim of reassessing the metallicity of Praesepe , and its difference ( if any ) with the Hyades cluster , we present in this paper a spectroscopic investigation of ten solar-type dwarf members .

Methods : We exploited GIARPS at the TNG to acquire high-resolution , high-quality optical and near-IR spectra and derived stellar parameters , metallicity ( [ Fe/H ] ) , light elements , \alpha - and iron-peak elements , by using a strictly differential ( line-by-line ) approach .
We also analysed in the very same way the solar spectrum and the Hyades solar analogue HD 28099 .

Results : Our findings suggest that Praesepe is more metal-rich than the Hyades , at the level of \Delta [ Fe/H ] =+0.05 \pm 0.01 dex , with a mean value of [ Fe/H ] =+0.21 \pm 0.01 dex .
All the other elements scale with iron , as expected .
This result seems to reject the hypothesis of a common origin for these two open clusters .
Most importantly , Praesepe is currently the most metal-rich , young open cluster living in the solar neighbourhood .

Conclusions :