  We present the first optical observations taken to characterize the
near-Earth object 138175 (2000 EE104). This body is associated with
Interplanetary Field Enhancements (IFEs), thought to be caused by interactions
between the solar wind magnetic field and solid material trailing in the orbit
of the parent body. Based on optical photometry, the radius (in meters) and
mass (in kilograms) of an equal-area sphere are found to be r_n =
250(0.1/p_R)**0.5 and M_n = 1e11(0.1/p_R)**1.5, respectively, where p_R is the
red geometric albedo and density 1500 kg/m3 is assumed. The measured colors are
intermediate between those of C-type (primitive) and S-type (metamorphosed)
asteroids but, with correction for the likely effects of phase-reddening, are
more consistent with a C-type classification than with S-type. No evidence for
co-moving companions larger than about 40(0.1/p_R) meter in radius is found,
and no dust particle trail is detected, setting a limit to the trail optical
depth 2e-9. Consideration of the size distribution produced by impact
pulverization makes it difficult to generate the mass of nanodust (minimum 1e5
kg to 1e6 kg) required to account for IFEs, unless the size distribution is
unusually steep. Furthermore, impact pulverization timescales for source
objects of the required size are much longer than the dynamical timescale.
While the new optical data do not definitively refute the hypothesis that
boulder pulverization is the source of IFEs, neither do they provide any
support for it.
