\begin{document}$\Delta r_{{np}}$\end{document}) of \begin{document}$ ^{48} {\rm{Ca}}$\end{document} nucleus, and astrophysical observations of the maximum masses of neutron stars. \begin{document}$\Delta r_{np}$\end{document} (\begin{document}$ ^{48} {\rm{Ca}}$\end{document}) = 0.146±0.019 fm is achieved with soft symmetry energy (\begin{document}$ J_{0} $\end{document} = 27.91±1.31 MeV) and its corresponding slope (\begin{document}$ L_{0} $\end{document} = 42.85±14.26 MeV) at saturation density. An equation of state (EoS) with a composition of β-equilibrated nucleonic and leptonic matter is computed. The nuclear matter and neutron star properties are also analyzed for this interaction and agree well with the astrophysical observations, such as the NICER and GW170817 events. We also perform a statistical analysis to estimate the theoretical errors in coupling parameters and neutron star observables and to determine the correlation coefficients. We observe that the neutron skins of \begin{document}$ ^{208} {\rm{Pb}}$\end{document} and \begin{document}$ ^{48} {\rm{Ca}}$\end{document} are strongly correlated and exhibit a strong dependence on \begin{document}$ J_{0} $\end{document}, \begin{document}$ L_{0} $\end{document} and the curvature of symmetry energy (\begin{document}$ K_{\text{sym}} $\end{document}) as suggested from their correlations. A strong correlation of canonical mass neutron star radius,\begin{document}$ R_{1.4} $\end{document} with ρ-meson-nucleon coupling quantified by the term \begin{document}$ g_{\rho N} $\end{document} and mixed interaction terms \begin{document}$ \sigma\rho_{\mu}\rho^{\mu} $\end{document} and \begin{document}$ \sigma^{2}\rho_{\mu}\rho^{\mu} $\end{document} is also observed."> Nuclear matter and neutron star properties constrained by CREX results and astrophysical constraints: A covariance study -
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