On the Nature of AGN and Star Formation Enhancement in the $z = 3.1$
  SSA22 Protocluster: The HST WFC3 IR View
  We examine possible environmental sources of the enhanced star formation and
active galactic nucleus (AGN) activity in the $z = 3.09$ SSA22 protocluster
using Hubble WFC3 F160W ($\sim1.6\ \rm \mu m$) observations of the SSA22 field,
including new observations centered on eight X-ray selected protocluster AGN.
To investigate the role of mergers in the observed AGN and star formation
enhancement, we apply both quantitative (S\'ersic-fit and Gini-$M_{20}$) and
visual morphological classifications to F160W images of protocluster Lyman
break galaxies (LBGs) in the fields of the X-ray AGN and $z \sim 3$ field LBGs
in SSA22 and GOODS-N. We find no statistically significant differences between
the morphologies and merger fractions of protocluster and field LBGs, though we
are limited by small number statistics in the protocluster. We also fit the
UV-to-near-IR spectral energy distributions (SED) of F160W-detected
protocluster and field LBGs to characterize their stellar masses and star
formation histories (SFH). We find that the mean protocluster LBG is by a
factor of $\sim2$ times more massive and more attenuated than the mean $z \sim
3$ field LBG. We take our results to suggest that ongoing mergers are not more
common among protocluster LBGs than field LBGs, though protocluster LBGs appear
to be more massive. We speculate that the larger mass of the protocluster LBGs
contributes to the enhancement of SMBH mass and accretion rate in the
protocluster, which in turn drives the observed protocluster AGN enhancement.
