  A set of hadronic equations of state (EoSs) derived from relativistic density
functional theory and constrained by terrestrial experiments, astrophysical
observations, in particular by the GW170817 event, and chiral effective field
theory ($\chi$EFT) of neutron matter is used to explore the sensitivity of the
EoS parameterization on the few nuclear matter characteristics defined at the
saturation density. We find that the gross properties of compact stars are most
sensitive to the isoscalar skewness coefficient $Q_{\text{sat}}$ and the
isovector slope coefficient $L_{\text{sym}}$ around saturation density, since
the higher order coefficients, such as $K_{\text{sym}}$, are fixed by our
model. More specifically, (i) among these $Q_{\text{sat}}$ is the dominant
parameter controlling both the maximum mass and the radii of compact stars
while $L_{\rm sym}$ is constrained somewhat by $\chi$EFT of neutron matter;
(ii) massive enough ($M\sim 2.0~M_{\odot})$ compact stars featuring both
hyperons and $\Delta$ resonances can be obtained if the value of
$Q_{\text{sat}}$ is large enough; (iii) the emergence of $\Delta$'s reduces the
radius of a canonical mass ($M\sim 1.4~M_{\odot})$ compact star thus easing the
tension between the predictions of the relativistic density functionals and the
inferences from the X-ray observation of nearby isolated neutron stars.
