# Fast and automated oscillation frequency extraction using Bayesian multi-modality

## TL;DR

This paper introduces a rapid Bayesian method for extracting individual oscillation mode frequencies in stars, achieving high precision and accuracy, which is crucial for analyzing large datasets from space missions like TESS and PLATO.

## Contribution

A novel, fast Bayesian approach building on previous methods to accurately determine stellar oscillation frequencies from space-based observations.

## Key findings

- Achieves frequency precision of about 0.1%
- Attains accuracy of about 0.01% compared to literature
- Effective for red giant branch stars

## Abstract

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.