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The neutron skin thickness $\Delta r_{\rm{np}}$ of heavy nuclei isessentially determined by the symmetry energy density slope $L({\rho })$ at$\rho_c = 0.11~{\rm {fm}^{-3}}\approx 2/3\rho_0$ ($\rho_0$ is nuclearsaturation density), roughly corresponding to the average density of finitenuclei. The PREX collaboration recently reported a model-independent extractionof $\Delta r^{208}_{\rm{np}} = 0.283 \pm 0.071$ fm for the $\Delta r_{\rm{np}}$of $^{208}$Pb, suggesting a rather stiff symmetry energy $E_{\rm{sym}}({\rho})$ with $L({\rho_c }) \ge 52$ MeV. We show that the $E_{\rm{sym}}({\rho })$cannot be too stiff and $L({\rho_c }) \le 73$ MeV is necessary to be compatiblewith (1) the ground-state properties and giant monopole resonances of finitenuclei, (2) the constraints on the equation of state of symmetric nuclearmatter at suprasaturation densities from flow data in heavy-ion collisions, (3)the largest neutron star (NS) mass reported so far for PSR J0740+6620, (4) theNS tidal deformability extracted from gravitational wave signal GW170817 and(5) the mass-radius of PSR J0030+045 measured simultaneously by NICER. Thisallows us to obtain $52 \le L({\rho_c }) \le 73$ MeV and $0.212 \le \Deltar^{208}_{\rm{np}} \le 0.271$ fm, and further $E_{\rm{sym}}({\rho_0 }) = 34.3\pm 1.7$ MeV, $L({\rho_0 }) = 83.1 \pm 24.7$ MeV, and $E_{\rm{sym}}({2\rho_0 })= 62.8 \pm 15.9$ MeV. A number of critical implications on nuclear physics andastrophysics are discussed.

Constraints on the Symmetry Energy from PREX-II in the Multimessenger Era