  In the era of state-of-the-art space-borne telescopes, high-resolution
ground-based observation has emerged as a crucial method for characterizing
exoplanets, providing essential insights into their atmospheric compositions.
In the optical and NIR regions, high-resolution spectroscopy has been powerful
for hot Jupiters (HJ) and ultra-hot Jupiters (UHJ) during their primary
transits, as it can probe molecules with better sensitivity. Here, we focus on
a comparative simulation study of WASP-76 b (UHJ) and WASP-77 A b (HJ) for
different number of transits, utilizing three ground-based spectrographs
(GIANO-B (TNG), CARMENES (CAHA), and ANDES (E-ELT)) with varying instrumental
parameters, spectral coverages, and resolutions. We aim to evaluate the
feasibility of the upcoming ground-based European Extremely Large Telescope
(E-ELT) in probing molecules from planet atmospheres and how it surpasses other
ground-based observatories in terms of detectability. With the 1-D model,
petitCODE, we have self-consistently simulated the atmospheric
pressure-temperature profiles, which are subsequently integrated into the 1-D
chemical kinetics model, VULCAN, to evolve the atmospheric chemistry.
High-resolution spectra are obtained by performing line-by-line radiative
transfer using petitRADTRANS. Finally, we use the resulting spectra to assess
the detectability (sigma_det) of molecular bands, employing the ground-based
noise simulator SPECTR. Utilizing cross-correlation spectroscopy, we have
successfully demonstrated the robust consistency between our simulation study
and real-time observations for both planets. ANDES excels overall in molecular
detection due to its enhanced instrumental architecture, reinforcing E-ELT's
importance for studying exoplanet atmospheres. Additionally, our theoretical
simulations predict the detection of CO, NH3, and H2S on WASP-76 b atmosphere
with a sigma_det> 3.
