  In several instances chemical abundances of dwarf and giant stars are used
simultaneously under the assumption that they share the same abundance scale.
This assumption might have implications in different astrophysical contexts. We
aim to ascertain a methodology capable of producing a consistent metallicity
scale for giants and dwarfs. To achieve that, we analyzed giants and dwarfs in
the Hyades open cluster. All these stars have archival high-resolution
spectroscopic data obtained with HARPS and UVES. In addition, the giants have
interferometric measurements of the angular diameters. We analyzed the sample
with two methods. The first method constrains the atmospheric parameters
independently from spectroscopy. For that we present a novel calibration of
microturbulence based on 3D model atmospheres. The second method is the
classical spectroscopic based on Fe lines. We also tested two line lists in an
attempt to minimize possible non-LTE effects and to optimize the treatment of
the giants. We show that it is possible to obtain a consistent metallicity
scale between dwarfs and giants. The preferred method should constrain the
three parameters $T_{\rm eff}$, $\log~g$, and $\xi$ independent of
spectroscopy. In particular, the lines should be chosen to be free of blends in
the spectra of giants. When attention is paid to the line list, the classical
spectroscopic method can also produce consistent results. The metallicities
derived with the well-constrained set of stellar parameters are consistent
independent of the line list used. Therefore, for this cluster we favor the
metallicity of +0.18$\pm$0.03 dex obtained with this method. The classical
spectroscopic analysis, using the line list optimized for the giants, provides
a metallicity of +0.14$\pm$0.03 dex, in agreement with previous works.
