Asteroseismic modelling of main-sequence solar-like stars and Kepler exoplanet host stars with the FICO procedure

I. Catalogue of fundamental stellar properties

¹ Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden
² LIRA, Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS, 92190 Meudon, France
³ STAR Institute, Université de Liège, Liège, Belgium
⁴ Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone, Italy
⁵ Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, P-4150-762 Porto, Portugal

^★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 23 September 2025
Accepted: 26 April 2026

Abstract

Context. 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.

Aims. We present detailed asteroseismic modelling of 95 main-sequence solar-like stars and Kepler 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.

Methods. 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.

Results. 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 Kepler LEGACY sample) that are comparable to the PLATO accuracy requirement of 10% for a Sun-like star. This is not negligible in that context.

Conclusions. 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.