We present 1.3 and 3 mm aperture synthesis imaging of the
  multiple T Tauri system UZ Tauri. UZ Tau is a hierarchical triple
  composed of a single star, UZ Tau E, 530 AU distant from a 50 AU
  binary, UZ Tau W.  Both dust and gas emission from the close binary
  are at least a factor of four lower than from the single star.  Since
  UZ Tau E and W have similar stellar masses, luminosities, and ages, we
  conclude that the mass of dust and gas associated with UZ Tau W is
  reduced solely by the influence of a close companion.  The disk
  emission from UZ Tau E is best interpreted as a circumstellar disk
  similar to those around other single T Tauri stars.  In a
  1"-resolution aperture synthesis map, CO (2-->1) emission is
  coincident with the continuum peak and elongated with a size of 300 AU
  (FWHM); a velocity gradient is seen along the long axis, consistent
  with rotation in a gaseous disk.  The emission is elongated at
  position angle 19 degrees, the same as the PA of previous polarization
  measurements.  A disk model fit to the continuum spectral energy
  distribution (SED) of UZ Tau E yields a disk mass of 0.06 M_sun.  In
  contrast, no CO emission is detected from UZ Tau W, and its 1.3 mm
  continuum emission is unresolved in a 1" (FWHM) beam (corresponding to
  a 70 AU radius).  The small extent of the emission and dynamical
  considerations imply that the 50 AU binary cannot be surrounded by any
  appreciable circumbinary disk; its mm-wave emission is from
  circumstellar disks around one or both components.  The mass of the
  circumstellar material is in the range 0.002--0.04 M_sun; the large
  uncertainty is due to the unknown temperature and surface density
  distributions of the material.  The properties of the UZ Tau E disk
  are similar to those inferred for the early solar nebula; such a disk
  could give rise to a planetary system like our own.  The mass of the
  UZ Tau W disk(s) is only marginally consistent with a ``minimum mass
  solar nebula.''  The constraints on disk size in UZ Tau W indicate
  that reduced mm-wave flux may be linked to a disparity in the size of
  disks (and therefore of planetary systems) around single and binary
  stars.