  Through continuous progress in nuclear theory and experiment and an
increasing number of neutron-star observations, a multitude of information
about the equation of state (EOS) for matter at extreme densities is available.
Here, we apply these different pieces of data individually to a broad set of
physics-agnostic candidate EOSs and analyze the resulting constraints.
Specifically, we make use of information from chiral effective field theory,
perturbative quantum chromodynamics, as well as data from heavy-ion collisions
and the PREX-II and CREX experiments. We also investigate the impact of current
mass and radius measurements of neutron stars, such as radio timing
measurements of heavy pulsars, NICER data, and other X-ray observations. We
augment these by reanalyses of the gravitational-wave (GW) signal GW170817, its
associated kilonova AT2017gfo and gamma-ray burst afterglow, the GW signal
GW190425, and the GRB211211A afterglow, where we use improved models for the
tidal waveform and kilonova light curves. Additionally, we consider the
postmerger fate of GW170817 and its consequences for the EOS. This large and
diverse set of constraints is eventually combined in numerous ways to explore
limits on quantities such as the typical neutron-star radius, the maximum
neutron-star mass, the nuclear symmetry-energy parameters, and the speed of
sound. Based on the priors from our EOS candidate set, we find the radius of
the canonical 1.4 M$_\odot$ neutron star to be $R_{1.4}= 12.27_{-0.94}^{+0.83}$
km and the TOV mass $M_{\rm TOV}= 2.26_{-0.22}^{+0.45}$ M$_\odot$ at 95%
credibility, when including those constraints where systematic uncertainties
are deemed small. A less conservative approach, combining all the presented
constraints, similarly yields $R_{1.4}= 12.20_{-0.50}^{+0.53}$ km and $M_{\rm
TOV}= 2.31_{-0.20}^{+0.08}$ M$_\odot$.
