  Since the advent of CoRoT, and NASA Kepler and K2, the number of low- and
intermediate-mass stars classified as pulsators has increased very rapidly with
time, now accounting for several $10^4$ targets. With the recent launch of NASA
TESS space mission, we have confirmed our entrance to the era of all-sky
observations of oscillating stars. TESS is currently releasing good quality
datasets that already allow for the characterization and identification of
individual oscillation modes even from single 27-days shots on some stars. When
ESA PLATO will become operative by the next decade, we will face the
observation of several more hundred thousands stars where identifying
individual oscillation modes will be possible. However, estimating the
individual frequency, amplitude, and lifetime of the oscillation modes is not
an easy task. This is because solar-like oscillations and especially their
evolved version, the red giant branch (RGB) oscillations, can vary
significantly from one star to another depending on its specific stage of the
evolution, mass, effective temperature, metallicity, as well as on its level of
rotation and magnetism. In this perspective I will present a novel, fast, and
powerful way to derive individual oscillation mode frequencies by building on
previous results obtained with \diamonds. I will show that the oscillation
frequencies obtained with this new approach can reach precisions of about 0.1 %
and accuracies of about 0.01 % when compared to published literature values for
the RGB star KIC~12008916.
