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In this empirical work, we aim to quantify the systematic uncertainties instellar mass $(M_\star)$ estimates made from spectral energy distribution (SED)fitting through stellar population synthesis (SPS), for galaxies in the localUniverse, by using the dynamical mass $(M_\text{dyn})$ estimator as anSED-independent check on stellar mass. We first construct a statistical modelof the high dimensional space of galaxy properties; size $(R_e)$, velocitydispersion $(\sigma_e)$, surface brightness $(I_e)$, mass-to-light ratio$(M_\star/L)$, rest-frame colour, S\'ersic index $(n)$ and dynamical mass$(M_\text{dyn})$; accounting for selection effects and covariant errors. Wedisentangle the correlations among galaxy properties and find that thevariation in $M_\star/M_\text{dyn}$ is driven by $\sigma_e$, S\'ersic index andcolour. We use these parameters to calibrate an SED-independent $M_\star$estimator, $\hat{M}_\star$. We find the random scatter of the relation$M_\star-\hat{M}_\star$ to be $0.108\text{dex}$ and $0.147\text{dex}$ forquiescent and star-forming galaxies respectively. Finally, we inspect theresiduals as a function of SPS parameters (dust, age, metallicity, starformation rate) and spectral indices (H$\alpha$, H$\delta$, $D_n4000)$. Forquiescent galaxies, $\sim65\%$ of the scatter can be explained by theuncertainty in SPS parameters, with dust and age being the largest sources ofuncertainty. For star-forming galaxies, while age and metallicity are theleading factors, SPS parameters account for only $\sim13\%$ of the scatter.These results leave us with remaining unmodelled scatters of $0.055\text{dex}$and $0.122\text{dex}$ for quiescent and star-forming galaxies respectively.This can be interpreted as a conservative limit on the precision in $M_\star$that can be achieved via simple SPS-modelling.

Galaxy And Mass Assembly (GAMA): Stellar-to-Dynamical Mass Relation I. Constraining the Precision of Stellar Mass Estimates