  The 3" pair of B9 stars, HD 28867, is one of the brightest X-ray sources in
the Taurus-Auriga star forming region. In this multi-wavelength study, we
attempt to deduce the source of the X-ray emission. We show that the East
component is the X-ray source. The East component has a near-IR excess and
displays narrow absorption lines in the optical, both of which are consistent
with a cool stellar companion. This companion is one of the brightest low mass
pre-main sequence stars in Tau-Aur; at 2 microns it and the B9 star are equally
bright. We see evidence for radial velocity variability in the cool component
of >34 km/s. It is not visible in K band speckle imaging, which constrains the
companion to lie within 14 AU of the B star.
  We also report on a possible fourth member of the group, an M1 star 18" south
of HD 28867.
