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An increasingly popular method to determine stellar ages of red-giant starsfor the purpose of Galactic archaeology is asteroseismic grid-based modelling(GBM). In asteroseismic GBM of red-giant stars with solar-like oscillations thelarge frequency separation ($\Delta\nu$) and the frequency of maximumoscillation power ($\nu_{\rm max}$) are commonly used asteroseismicobservables, in addition to the usual spectroscopic parameters effectivetemperature ($T_{\rm eff}$) and metallicity ([Fe/H]). The precision with which$\Delta\nu$ and $\nu_{\rm max}$ can be determined largely depends on the lengthof the timeseries data (assuming the stars are bright enough that theoscillations can be detected). The question that we aim to answer here is: withwhat precision should [Fe/H] and $T_{\rm eff}$ be obtained to derive stellarages of red-giant stars through asteroseismic GBM given the precision of$\Delta\nu$ and $\nu_{\rm max}$ that we can expect from the TESS data? In mostcases presented here the value of $\sigma_{\rm age}$ shows only weak, or no,dependence on the uncertainties and biases in [Fe/H] and $T_{\rm eff}$ ingestedin this study. Only in case a large ($>100$~K) $T_{\rm eff}$ biases isaccompanied by a small (50 K) uncertainties in $T_{\rm eff}$ on the red-giantbranch, $\Delta_{\rm age}$ is of the order of or larger than $\sigma_{\rm age}$and in these cases we expect an impact of this bias on the resulting ageestimate.

Asteroseismic ages of red-giant stars from grid-based modelling: the impact of systematics in effective temperature or metallicity