  The so-called Nysa-Polana complex of asteroids is a diverse and widespread
group. It appears to be two overlapping families of different asteroid
taxonomies: (44) Nysa is an E-type asteroid with the lowest number in the midst
of a predominantly S-type cluster and (142) Polana is a B-type asteroid near
the low-albedo B- and C-type cluster.
  Using the data from the Wide-field Infrared Survey Explorer (WISE) mission we
have re-analyzed the region around the Nysa-Polana complex in the inner Main
Belt, focusing on the low-albedo population. (142) Polana does not appear to be
a member of the family of low-albedo asteroids in the Nysa-Polana complex.
Rather, the largest is asteroid (495) Eulalia. This asteroid has never before
been linked to this complex for an important dynamical reason: it currently has
a proper eccentricity slightly below the range of most of the family members.
However, its orbit is very close to the 3:1 mean motion resonance with Jupiter
and is in a weak secular resonance. We show that its osculating eccentricity
varies widely on short timescales and the averaged value diffuses over long
timescales. The diffusive orbit, low-albedo, taxonomic similarity and semimajor
axis strongly suggests that despite its current proper eccentricity, (495)
Eulalia could have recently been at an orbit very central to the family.
Hierarchical Clustering Method tests confirm that at an eccentricity of e=0.15,
(495) Eulalia could be the parent of the family. The ``Eulalia family'' was
formed between 900--1500 Myr ago, and likely resulted from the breakup of a
100--160 km parent body. There is also compelling evidence for an older and
more widespread primitive family in the same region of the asteroid belt
parented by asteroid (142) Polana.
