  Perhaps as many as 10% of high redshift radio galaxy (HzRG; z > 2) candidates
that are selected using an Ultra Steep radio Spectrum (USS) criterion fail to
show optical emission (continuum, lines) in deep Keck exposures. Their parent
objects are only detected in the near-IR and are probably heavily obscured
and/or at very high redshift. To search for signatures of dust and help
constrain the nature and redshifts of these ``no-z'' radio galaxies, we have
conducted a program of submillimeter and millimeter observations. Here we
report the first results of a detailed study of one of these objects, WN
J0305+3525.
  WN J0305+3525 appears associated with a small group of K ~ 21 - 22 objects
and is strongly detected at both 850 micron and 1.25 mm. On the basis of its
faint K-band magnitude, spectral energy distribution (SED) and other evidence
we estimate that the radio galaxy is probably at a redshift z = 3 +/- 1. This
would make WN J0305+3525 a radio-loud Hyper Luminous Infrared Galaxy (LFIR ~
10^13 Lsun) similar to, but more obscured than, other dusty radio galaxies in
this redshift range. This, together with the absence of Lya emission and
compact (theta < 1.9") radio structure, suggests that WN J0305+3525 is embedded
in a very dense, dusty medium and is probably at an early stage of its
formation.
