Is a 1D perturbative method sufficient for asteroseismic modelling of β Cephei pulsators?

Supplementary material for Mombarg et al. (2025, A&A). Title: "Is a 1D perturbative method sufficient for asteroseismic modelling of $\beta$~Cephei pulsators? Implications for measurements of rotation and internal magnetic fields" Content:- Non-rotating ESTER models and associated .GSM models. (Xini = 0.71, Zini = 0.014, vertical/horizonal viscosity 10^7 cm^2/s, vertical chemical diffusion 10^4 cm^2/s for evolution model. More details on the ESTER models can be found in the ESTER manual. - Rotational asymmetries computed with StORM and TOP in 1/d, and the central m=0 frequency from TOP in 1/d. (all_A*_new.pkl) - Magnetic asymmetries in 1/d for different obliquity angles between 0 and 90 deg for ZAMS and MAMS model, for B_0 = 75 kG. *_nu key gives unperturbed mode frequencies, *_npg the radial order (asym_dict.pkl, asym_dict_evol.pkl)