Clustering with JWST: Constraining Galaxy Host Halo Masses, Satellite
  Quenching Efficiencies, and Merger Rates at z=4-10
  Galaxy clustering measurements can be used to constrain many aspects of
galaxy evolution, including galaxy host halo masses, satellite quenching
efficiencies, and merger rates. We simulate JWST galaxy clustering measurements
at z$\sim$4$-$10 by utilizing mock galaxy samples produced by an empirical
model, the UniverseMachine. We also adopt the survey footprints and typical
depths of the planned joint NIRCam and NIRSpec Guaranteed Time Observation
program planned for Cycle 1 to generate realistic JWST survey realizations and
to model high-redshift galaxy selection completeness. We find that galaxy
clustering will be measured with $\gtrsim$5$\sigma$ significance at
z$\sim$4$-$10. Halo mass precisions resulting from Cycle 1 angular clustering
measurements will be $\sim$0.2 dex for faint (-18 $\gtrsim$
$\mathit{M}_{\mathrm{UV}}^{ }$ $\gtrsim$ -19) galaxies at z$\sim$4$-$10 as well
as $\sim$0.3 dex for bright ($\mathit{M}_{\mathrm{UV}}^{ }$ $\sim$ -20)
galaxies at z$\sim$4$-$7. Dedicated spectroscopic follow-up over $\sim$150
arcmin$^2$ would improve these precisions by $\sim$0.1 dex by removing chance
projections and low-redshift contaminants. Future JWST observations will
therefore provide the first constraints on the stellar-halo mass relation in
the epoch of reionization and substantially clarify how this relation evolves
at z$>$4. We also find that $\sim$1000 individual satellites will be
identifiable at z$\sim$4$-$8 with JWST, enabling strong tests of satellite
quenching evolution beyond currently available data (z$\lesssim$2). Finally, we
find that JWST observations can measure the evolution of galaxy major merger
pair fractions at z$\sim$4$-$8 with $\sim$0.1$-$0.2 dex uncertainties. Such
measurements would help determine the relative role of mergers to the build-up
of stellar mass into the epoch of reionization.
