Bolometric corrections of stellar oscillation mode amplitudes as observed by the PLATO mission

I. Planck-spectrum estimates

¹ Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
² Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, CNES, 14 avenue Edouard Belin, 31400 Toulouse, France
³ School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK

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

Received: 18 December 2025
Accepted: 9 March 2026

Abstract

Aims. We derive bolometric correction functions for oscillation mode amplitudes observed by the different cameras of the ESA PLATO mission. Such corrections between bolometric (full light) and mission instrument-specific amplitudes enable comparisons to theoretical expectations and amplitude conversion between different photometric missions, which is essential for proper detectability yields and target selection.

Methods. Bolometric correction functions were calculated assuming a Planck function approximation for the stellar spectral flux distribution. The calculations follow the procedures applied in earlier analyses for the NASA Kepler and TESS missions. We derived power-law and polynomial parametrisations of the bolometric corrections with T_eff.

Results. We find that on average, oscillation mode amplitudes from PLATO’s normal cameras (N-CAMs) are expected to be ∼6.7% lower compared to Kepler, and ∼12.5% higher compared to TESS. A significant average amplitude ratio of ∼25% is expected for amplitudes measured using the blue PLATO fast camera (F-CAM) compared to TESS. We find that observations of bright solar-like oscillators, especially with PLATO’s F-CAMs, would provide an important test of the predicted corrections.