Implications of the Environments of Radio-detected AGN in a Complex
  Protostructure at z$\sim$3.3
  Radio Active Galactic Nuclei (RAGNs) are mainly found in dense structures
(i.e., clusters/groups) at redshifts of z$<$2 and are commonly used to detect
protoclusters at higher redshift. Here, we attempt to study the host and
environmental properties of two relatively faint ($\mathrm L_\mathrm{1.4GHz}
\sim10^{25}$ W Hz$^{-1}$) RAGNs in a known protocluster at z=3.3 in the PCl
J0227-0421 field, detected using the latest radio observation obtained as part
of the Observations of Redshift Evolution in Large-Scale Environments (ORELSE)
Survey. Using new spectroscopic observations obtained from Keck/MOSFIRE as part
of the Charting Cluster Construction with the VIMOS Ultra-Deep Survey (VUDS)
and ORELSE (C3VO) survey and previous spectroscopic data obtained as part of
the VIMOS-VLT Deep Survey (VVDS) and VUDS, we revise the three-dimensional
overdensity field around this protocluster. The protocluster is embedded in a
large scale overdensity protostructure. This protostructure has an estimated
total mass of $\sim$2.6$\times10^{15} M_\odot$ and contains several overdensity
peaks. Both RAGNs are hosted by very bright and massive galaxies, while their
hosts show extreme differences color, indicating that they have different ages
and are in different evolutionary stages. Furthermore, we find that they are
not in the most locally dense parts of the protostructure, but are fairly close
to the centers of their parent overdensity peaks. We propose a scenario where
merging might already have happened in both cases, which lowered the local
density of their surrounding area and boosted their stellar mass. This work is
the first time that two RAGNs at low luminosity have been found and studied
within a high redshift protostructure.
