Asteroseismology has revolutionised our ability to characterise solar-like stars. Since asteroseismic modelling is a key factor in upcoming space-based missions such as PLATO, it becomes increasingly relevant to develop robust and scalable modelling techniques for the precise and accurate characterisation of main-sequence and exoplanet host stars in the PLATO era. We present detailed asteroseismic modelling of 95 main-sequence solar-like stars and exoplanet host stars using the Forward and Inverse COmbination (FICO) procedure, a three-step method that combines forward and inverse techniques, which enables the precise inference of fundamental stellar parameters such as mass, radius, age, and mean density. These results are then discussed in the framework of the PLATO mission. Kepler We applied the FICO procedure to a catalogue of nearly 100 stars with high-quality asteroseismic and classical observations and compared its results against literature values. We also compared its performance with direct frequency fitting using semi-empirical surface corrections. The FICO procedure achieved statistical precisions of 2. 3%, 0. 82%, 6. 9%, and 0. 49% in mass, radius, age, and mean density, respectively, on average. This is well within PLATO quality requirements. We reconfirmed that surface-independent methods more effectively mitigate biases inherent to semi-empirical surface corrections, particularly for stars more massive than 1. 15 M_⊙ or above 6050 K. Two regimes were identified: near-solar conditions, where the two approaches perform similarly, and higher-mass stars, where surface-independent methods consistently outperform direct fitting methods. While our results are consistent with literature values, we observed age biases (∼ 11. 5% on average for the LEGACY sample) that are comparable to the PLATO accuracy requirement of 10% for a Sun-like star. This is not negligible in that context. Kepler The FICO procedure provides a robust framework for high-precision stellar characterisation in the PLATO era. Its hybrid architecture effectively addresses surface effects, making it a promising tool for the accurate determination of exoplanet host-star properties. Our findings also highlight the importance of carefully selecting and validating the physical assumptions embedded in stellar models, particularly in the context of next-generation space missions such as PLATO.
Bétrisey et al. (Wed,) studied this question.