We present phase-referenced VLBI results on the radio continuum and the OH 18 cm megamaser emission from the Ultra-Luminous Infrared Galaxy , IRAS 17208–0014 . The observations were carried out at 1599 MHz using the Very Long Baseline Array , the phased VLA , and the Green Bank Telescope . The highest resolution radio continuum results show several compact sources with brightness temperatures on the order of 10 ^ { 6 } K. These sources are more likely to be clustered supernova remnants and/or luminous radio supernovae . However , the agreement between the number of observed and expected compact sources above the 5 \sigma level supports the possibility that each one of the compact sources could be dominated by a recently detonated luminous radio supernova . The continuum results suggest that there is no radio-loud AGN in the nuclear region of this galaxy . The OH 18 cm megamaser emission in IRAS 17208–0014 is detected at various angular resolutions . It has an extent of 170 \times 110 pc , and is mostly localized in two regions separated by 61 pc . The structure and dynamics of the maser emission seem to be consistent with a clumpy , rotating , ring-like geometry , with the two dominant maser regions marking the tangential points of the proposed rotating-ring distribution . Assuming Keplerian motion for the rotating maser ring , the enclosed dynamical mass and the mass density within a radius of 30.5 pc , are about 3 \times 10 ^ { 7 } ~ { } ( { sin } ^ { -2 } i ) ~ { } M { { } _ { \odot } } , and 281 ~ { } ( { sin } ^ { -2 } ~ { } i ) ~ { } M { { } _ { \odot } } ~ { } { pc } ^ { -3 } , respectively .