We report the detection of an intriguing parsec-scale radio source in the “ offset AGN ” candidate , KISSR 102 . The elliptical host galaxy includes two optical nuclei at a projected separation of 1.54 kpc , N1 and N2 , to the south-east and north-west , respectively . Phase-referenced VLBA observations at 1.5 and 4.9 GHz of this LINER galaxy , have detected double radio components ( A and B ) at a projected separation of 4.8 parsec at 1.5 GHz , and another partially-resolved double radio structure at 4.9 GHz coincident with the brighter radio component A . These radio detections are confined to the optical nucleus N1 . The brightness temperatures of all the detected radio components are high , \gtrsim 10 ^ { 8 } K , consistent with them being components of a radio AGN . The 1.5 - 4.9 GHz spectral index is inverted ( \alpha \sim + 0.64 \pm 0.08 ) for component A and steep for component B ( \alpha \lesssim - 1.6 ) . The dramatic change in the spectral indices of A and B is inconsistent with it being a typical “ core-jet ” structure from a single AGN , or the mini-lobes of a compact symmetric object . To be consistent with a “ core-jet ” structure , the jet in KISSR 102 would need to be undergoing strong jet-medium interaction with dense surrounding media resulting in a drastic spectral steepening of the jet . Alternatively , the results could be consistent with the presence of a parsec-scale binary radio AGN , which is the end result of a three-body interaction involving three supermassive black holes in the center of KISSR 102 .