  Thanks to the recent advancement in producing rare isotopes and measuring
their masses with unprecedented precision, the updated nuclear masses around
the waiting-point nucleus $^{64}$Ge in the rapid-proton capture process have
led to a significant revision of the surface gravitational redshift of the
neutron star (NS) in GS 1826-24 by re-fitting its X-ray burst light curve ({\it
X. Zhou et al., Nature Physics {\bf 19}, 1091 (2023)}) using Modules for
Experiments in Stellar Astrophysics (MESA). The resulting NS compactness $\xi$
is between 0.244 and 0.342 at 95\% confidence level and its upper boundary is
significantly smaller than the maximum $\xi$ previously known. Incorporating
this new data within a comprehensive Bayesian statistical framework, we
investigate its impact on the Equation of State (EOS) of supradense
neutron-rich matter and the required spin frequency for GW190814's minor $m_2$
with mass $2.59\pm 0.05$M$_{\odot}$ to be a rotationally stable pulsar. We
found that the EOS of high-density symmetric nuclear matter (SNM) has to be
softened significantly while the symmetry energy at supersaturation densities
stiffened compared to our prior knowledge from earlier analyses using data from
both astrophysical observations and terrestrial nuclear experiments. In
particular, the skewness $J_0$ characterizing the stiffness of high-density SNM
decreases significantly, while the slope $L$, curvature $K_{\rm{sym}}$, and
skewness $J_{\rm{sym}}$ of nuclear symmetry energy all increase appreciably
compared to their fiducial values. We also found that the most probable spin
rate for the $m_2$ to be a stable pulsar is very close to its mass-shedding
limit once the revised redshift data from GS 1826-24 is considered, making the
$m_2$ unlikely the most massive NS observed so far.
