  In this study I assess how existing data for the solar analogues 16 Cyg A and
B, in particular the asteroseismic measurements obtained from \emph{Kepler},
constrain theoretical stellar models. The goal is two-fold: first to use these
stars as benchmarks to discuss which precisions can realistically be expected
on the inferred stellar quantities; and second to determine how well
'non-standard' prescriptions, such as microscopic diffusion and overshoot, are
constrained. I used a Bayesian statistical model to infer the values of the
stellar parameters of 16 Cyg A and B. I sampled the posterior density of the
stellar parameters via a Markov chain Monte Carlo (MCMC) algorithm, tested
different physical prescription, and examined the impact of using different
seismic diagnostics. General good agreement is found with several recent
modelling studies on these stars, even though some discrepancies subsist
regarding the precise estimates of the uncertainties on the parameters. An age
of $6.88\pm0.12$ Gyr is estimated for the binary system. The inferred masses,
$1.07\pm0.02$ M$_{\odot}$ for Cyg A and $1.05\pm0.02$ M$_{\odot}$ for Cyg B,
are shown to be stable with respect to changes in the physical prescriptions
considered for the modelling. For both stars, microscopic diffusion has a
significant effect on the estimates of the initial metallicity. Overshoot is
confined to very small regions below the convective zone. I show that a proper
treatment of the seismic constraints is necessary to avoid biases in the
estimate of the mass.
