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The so-called Nysa-Polana complex of asteroids is a diverse and widespreadgroup. It appears to be two overlapping families of different asteroidtaxonomies: (44) Nysa is an E-type asteroid with the lowest number in the midstof a predominantly S-type cluster and (142) Polana is a B-type asteroid nearthe low-albedo B- and C-type cluster.  Using the data from the Wide-field Infrared Survey Explorer (WISE) mission wehave re-analyzed the region around the Nysa-Polana complex in the inner MainBelt, focusing on the low-albedo population. (142) Polana does not appear to bea member of the family of low-albedo asteroids in the Nysa-Polana complex.Rather, the largest is asteroid (495) Eulalia. This asteroid has never beforebeen linked to this complex for an important dynamical reason: it currently hasa 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 Jupiterand is in a weak secular resonance. We show that its osculating eccentricityvaries widely on short timescales and the averaged value diffuses over longtimescales. The diffusive orbit, low-albedo, taxonomic similarity and semimajoraxis 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'' wasformed between 900--1500 Myr ago, and likely resulted from the breakup of a100--160 km parent body. There is also compelling evidence for an older andmore widespread primitive family in the same region of the asteroid beltparented by asteroid (142) Polana.

Introducing the Eulalia and new Polana asteroid families: re-assessing primitive asteroid families in the inner Main Belt