  We discuss the possibility of using OH and H2O gigamasers to trace the
redshift distribution of luminous, dust-obscured, star-forming galaxies. It has
long been thought that ultraluminous, interacting galaxies should host
gigamasers due to their vast pumping IR luminosity, the large column density of
molecules available to populate the maser states and the turbulent motion of
the gas in these dynamically complex systems which allows unsaturated maser
emission. OH masers may thus be well-suited to the redshift-blind detection of
ultraluminous and hyperluminous infrared galaxies (L_FIR >= 10^12 L_sun) such
as those uncovered by the SCUBA submillimetre camera. The bandwidth requirement
is low, <1 GHz for z=1-10 (lower still if additional redshift constraints are
available) and the dual-line 1665-/1667-MHz OH spectral signature can act as a
check on the reality of detections.
