  Pulse profile modeling of X-ray data from NICER is now enabling precision
inference of neutron star mass and radius. Combined with nuclear physics
constraints from chiral effective field theory ($\chi$EFT), and masses and
tidal deformabilities inferred from gravitational wave detections of binary
neutron star mergers, this has lead to a steady improvement in our
understanding of the dense matter equation of state (EOS). Here we consider the
impact of several new results: the radius measurement for the 1.42$\,M_\odot$
pulsar PSR J0437$-$4715 presented by Choudhury et al. (2024), updates to the
masses and radii of PSR J0740$+$6620 and PSR J0030$+$0451, and new $\chi$EFT
results for neutron star matter up to 1.5 times nuclear saturation density.
Using two different high-density EOS extensions -- a piecewise-polytropic (PP)
model and a model based on the speed of sound in a neutron star (CS) -- we find
the radius of a 1.4$\,M_\odot$ (2.0$\,M_\odot$) neutron star to be constrained
to the 95\% credible ranges $12.28^{+0.50}_{-0.76}\,$km
($12.33^{+0.70}_{-1.34}\,$km) for the PP model and $12.01^{+0.56}_{-0.75}\,$km
($11.55^{+0.94}_{-1.09}\,$km) for the CS model. The maximum neutron star mass
is predicted to be $2.15^{+0.14}_{-0.16}\,$$M_\odot$ and
$2.08^{+0.28}_{-0.16}\,$$M_\odot$ for the PP and CS model, respectively. We
explore the sensitivity of our results to different orders and different
densities up to which $\chi$EFT is used, and show how the astrophysical
observations provide constraints for the pressure at intermediate densities.
Moreover, we investigate the difference $R_{2.0} - R_{1.4}$ of the radius of
2$\,M_\odot$ and 1.4$\,M_\odot$ neutron stars within our EOS inference.
