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Being able to assess the presence of solar-like oscillations in stellar power spectra is a pre-requisite to any seismic analysis. Given the increasing harvest of ligthcurves obtained by the space missions Kepler, TESS, and in the coming years, PLATO, it is crucial to have a fast, robust and automated tool at hand. We developed a new pipeline allowing the Fast, Robust and Automated (FRA) detection of solar-like oscillations. It is based on the detection and measurement of the frequency of maximum oscillation power, νmax, and runs in a few seconds of CPU time. Our pipeline allows to measure νmax independently from the large separation, ∆ν, while using statistical criteria to validate or not the obtained measurement, and thus confirm or not the presence of oscillations. I present here the results we obtain when applying the FRA pipeline to ∼ 1700 Kepler and ∼ 2300 TESS red giants, as well as ∼ 250 artificial power spectra representative of TESS red giants. The analysis of artificial power spectra provides limits in magnitude and in the number of observed sectors required to obtain consistent νmax measurements, while maximizing the detectability of oscillations and minimizing the false positive detections. Since νmax is among the crucial seismic parameters to derive precise and accurate stellar masses and radii, the FRA pipeline represents a huge potential for Galactic archeology and exoplanet characterization.

Information on stellar inclinations are of prime importance to characterize the formation and dynamics of transiting exoplanetarysystems, by helping to constrain the angle between the stellar spin axis and the planetaryorbit axis, namely theobliquity. As PLATO will observe about 150 000 main-sequence stars potentially hostingexoplanets, it is crucial to have at hand afast, robust and automated method to measure the stellar inclination angle. I will present the method I developed and the results I derived for almost 1200 red giant stars that have beenobserved by the Keplerspace mission, which exhibit mixed modes offering the opportunity to obtain accurate measurements of the inclination angleof the stellar rotation axis. I could characterize the biases affecting inclinationmeasurements, in particular for extreme valuesclose to 0 ◦ and 90 ◦ . This study allowed me to provide a way to inferthe underlying statistical distribution of inclinations for agiven sample of stars, free from observational limitations.This method has the advantage to be able to deriveseismicmeasurements of theinclination angle for any solar-typepulsator with identified oscillation modes.

Red giant stars are solar-like pulsators presenting mixed-modes. Such modes consist in a coupling between pressure waves propagating in the external convective envelope and gravity waves propagating in the radiative interior. Therefore, the red giant asteroseismology provides us with a direct view on their core and opens the possibility to monitor the evolution of their core rotation. Previous measurements of the mean core rotation revealed that angular momentum is efficiently transferred from the core to the envelope inside red giants, but the physical mechanisms at work are not yet fully understood. We thus need stronger observational constraints on the evolution of the red giant core rotation. In this context, we developed an automated method to determine the mean core rotation of red giant branch stars observed with Kepler. This automated method is paving the way for the future PLATO data, representing hundreds of thousands of potential red giant oscillation spectra. Results obtained for almost 1200 red giant branch stars indicate that the rate of the core rotation braking is lower than previously estimated and does not seem to depend on the stellar mass., 5 pages, 3 figures, 2 tables, SF2A 2017