  Based on the Skyrme-Hartree-Fock model (SHF) as well as its extension (the
Korea-IBS-Daegu-SKKU (KIDS) model) and the relativistic mean-field (RMF) model,
we have studied the constraints on the parameters of the nuclear matter
equation of state (EOS) from adopted astrophysical observables using a Bayesian
approach. While the masses and radii of neutron stars generally favors a stiff
isoscalar EOS and a moderately soft nuclear symmetry energy, model dependence
on the constraints is observed and mostly originates from the incorporation of
higher-order EOS parameters and difference between relativistic and
non-relativistic models. At twice saturation density, the value of the symmetry
energy is constrained to be $48^{+15}_{-11}$ MeV in the standard SHF model,
$48^{+8}_{-15}$ MeV in the KIDS model, and $48^{+5}_{-6}$ MeV in the RMF model,
around their maximum {\it a posteriori} values within $68\%$ confidence
intervals. Our study helps to obtain a robust constraint on nuclear matter EOS,
and meanwhile, to understand the model dependence of the results.
