Modelling astroseismically known stars by searching for best-fitting models in stellar grids naturally depends on the number and precision of known stellar parameters, limiting the range of acceptable models. Here, we compare the solutions of such grid-based analyses of the seismic benchmark object 16 Cyg A+B as obtained using the approach of Nsamba et al. (2021), with an updated search including a Gaia-based luminosity (Yildiz et al. 2017). We repeat the exercise for α Cen A, the object with unknown core structure (radiative or convective; Nsamba et al. 2018), using either a parallax-based luminosity (Kervella et al. 2017) or the stellar radius as obtained from interferometry (Kervella et al. 2003) to restrict the space of possible solutions.