  Context: Asteroseismology, a powerful approach for obtaining internal
structure and stellar properties, requires surface temperature and chemical
composition information to determine mass and age. High-resolution spectroscopy
is a valuable technique for precise stellar parameters (including surface
temperature) and chemical composition analysis. Aim: We aim to combine
spectroscopic parameters with asteroseismology to test stellar models. Method:
Using high-resolution optical and near-IR spectra from GIARPS at the Telescopio
Nazionale Galileo, we conducted a detailed spectroscopic analysis of 16 stars
photometrically selected to be on the red giant and red clump. Stellar
parameters and chemical abundances for light elements (Li, C, N, F), Fe peak,
$\alpha$ and n-capture elements were derived using a combination of equivalent
widths and spectral synthesis techniques, based on atomic and molecular
features. Ages were determined through asteroseismic scaling relations and
compared with ages based on chemical clocks, [Y/Mg] and [C/N]. Results:
Spectroscopic parameters confirmed the stars as part of the red giant branch
and red clump. Two objects, HD 22045 and HD 24680 exhibited relatively high Li
abundances, with HD 24680 potentially being a Li-rich giant resulting from mass
transfer with an intermediate-mass companion, which already underwent its AGB
phase. Stellar parameters derived from scaling different sets of relations were
consistent with each other. For what concerns ages, the values based on
asteroseismology were in excellent agreement with those derived from
theoretical evolutionary tracks, but did not align with ages derived from the
chemical clocks [Y/Mg] and [C/N].
