  We present a new study of remnant black hole properties from 13 binary black
hole systems, numerically evolved using the Spectral Einstein Code. The mass,
spin, and recoil velocity of each remnant were determined quasi-locally from
apparent horizon data and asymptotically from Bondi data $(h, \psi_4, \psi_3,
\psi_2, \psi_1)$ computed at future null infinity using SpECTRE's Cauchy
characteristic evolution. We compare these independent measurements of the
remnant properties in the bulk and on the boundary of the spacetime, giving
insight into how well asymptotic data are able to reproduce local properties of
the remnant black hole in numerical relativity. We also discuss the theoretical
framework for connecting horizon quantities to asymptotic quantities and how it
relates to our results. This study recommends a simple improvement to the
recoil velocities reported in the Simulating eXtreme Spacetimes waveform
catalog, provides an improvement to future surrogate remnant models, and offers
new analysis techniques for evaluating the physical accuracy of numerical
simulations.
