Testing the Detection Significance on the Large Scale Structure by a JWST Deep Field Survey

In preparation for deep extragalactic imaging with the James Webb Space Telescope, we explore the clustering of massive halos at $z=8$ and $10$ using a large N-body simulation. We find that halos with masses ${10}^9$ to ${10}^{11}$ $h^{-1}{M}_{\odot }$, which are those expected to host galaxies detectable with JWST, are highly clustered with bias factors ranging from 5 and 30 depending strongly on mass, as well as on redshift and scale. This results in correlation lengths of 5–10$h^{-1}\mathrm{M}\mathrm{p}\mathrm{c}$, similar to that of today’s galaxies. Our results are based on a simulation of 130 billion particles in a box of $250h^{-1}\mathrm{M}\mathrm{p}\mathrm{c}$ size using our new high-accuracy ABACUS simulation code, the corrections to cosmological initial conditions of (Garrison et al. 2016, 2016MNRAS.461.4125G), and the Planck 2015 cosmology. We use variations between sub-volumes to estimate the detectability of the clustering. Because of the very strong inter-halo clustering, we find that surveys of order 25$h^{-1}\mathrm{M}\mathrm{p}\mathrm{c}$ comoving transverse size may be able to detect the clustering of $z=8$–$10$ galaxies with only 500-1000 survey objects if the galaxies indeed occupy the most massive dark matter halos.