  We use halo dwarf stars with photometrically determined metallicities that
are located within 2 kpc of the Sun to identify local halo substructure. The
kinematic properties of these stars do not indicate a single, dominant radial
merger event (RME). The retrograde Virgo Radial Merger (VRM) component has
[Fe/H] = -1.7. A second, non-rotating RME component we name Nereus is
identified with [Fe/H] = -2.1 and has similar energy as the VRM. A possible
third RME we name Cronus is identified that is co-rotating with the disk, has
lower energy than the VRM, and has [Fe/H] = -1.2. We identify the Nyx Stream in
the data. In addition to these substructures, we observe metal-poor halo stars
([Fe/H] ~ -2.0 and $\sigma_v$ ~ 180 km s$^{-1}$) and a disk/Splash component
with lower rotational velocity than the disk and lower metallicity than
typically associated with the Splash. An additional excess of halo stars with
low velocity and metallicity of [Fe/H] = -1.5 could be associated with the
shell of a lower energy RME or indicate that lower energy halo stars have
higher metallicity. Stars which comprise the "Gaia Sausage" velocity structure
are a combination of the components identified in this work.
