We present radio through X-ray results of a bright ( > 10 ^ { 40 } ergs s ^ { -1 } in the 0.5 to 8.0 keV band ) ultraluminous X-ray source ( ULX ) , CXOU J153434.9+151149 , in the starburst , interacting pair of galaxies NGC 5953/5954 . Chandra image of this ULX shows that it is elongated .
From HST/WFPC2/F606W data we have detected a counterpart of the ULX system with M _ { F 606 W } \sim -7.1 \pm 0.7 mag .
This optical counterpart may be either an O-type supergiant star or a young star cluster .
From our Fabry-Perot interferometric observations , we have detected H \alpha and [ NII ] ( \lambda 6584 Å ) diffuse emission , with velocity gradients up to 60 km s ^ { -1 } at the astrometric corrected Chandra position of the ULX .
Different scenarios have been invoked as to explain the possible nature of CXOU J153434.9+151149 .
Based on the observed X-ray morphology of the ULX , we determine that the inclination angle to the elongated emission will be \sim 53 ^ { o } .
Beaming with this geometry from a stellar-mass black hole system will be inadequate to explain the observed X-ray luminosity of this ULX .
Finally , we suggest that mild-beaming from a binary black hole with mass more than 50M _ { \odot } associated with a young star cluster , is the most favorable scenario that describes the multiwavelength properties of this ULX .
Future observations are highly essential to determine the nature of this rare object .