Stellar population astrophysics (SPA) with the TNG. Revisiting the
  metallicity of Praesepe (M44)
  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.
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. 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. Our findings suggest that Praesepe is more metal-rich than
the Hyades, at the level of $\Delta$[Fe/H]=+0.05$\pm$0.01 dex, with a mean
value of [Fe/H]=+0.21$\pm0.01$ 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.
