ETHANE PLAYS AN IMPORTANT ROLE IN THE HYDROLOGICAL CYCLE OF TITAN'S LIQUID HYDROCARBONS. IT IS LESS VOLATILE THAN METHANE BUT ALSO MORE SOLUBLE; THUS THE PRESENCE OF ETHANE WITHIN A LAKE OR SEA AFFECTS THE EVOLUTION OF THE BODY. WE PROPOSE TO USE DATA FROM THE CASSINI VISUAL AND INFRARED MAPPING SPECTROMETER (VIMS) TO DETERMINE WHERE ETHANE IS PRESENT IN TITAN'S LAKES AND SEAS. OUR RESULTS WOULD COMPLEMENT THE HANDFUL FOR COMPOSITION MEASUREMENTS CONDUCTED BY CASSINI RADAR PROVIDING REGIONAL CONTEXT FOR THOSE RESULTS. FURTHERMORE WE WILL EXPLORE WHETHER THE PRESENCE OF ETHANE IS HETEROGENOUS ACROSS THE SURFACE OF CERTAIN LAKES OR SEAS INCREASING OUR UNDERSTANDING OF THE FEASIBILITY OF HYPOTHESIZED INTERNAL LACUSTRINE PROCESSES LIKE MIXING OR SEDIMENT DEPOSITION. WE WILL USE THE 2 UM ABSORPTION FEATURE TO IDENTIFY THE PRESENCE OF ETHANE IN TITAN'S NORTH POLAR LAKES AND SEAS IN VIMS DATA FROM 2009-2015. WE WILL ALSO USE A FULLY SPHERICAL RADIATIVE TRANSFER CODE TO MODEL THE ADJACENCY EFFECT WHICH WE HYPOTHESIZE CREATES ARTIFICIAL BRIGHTENING AT THE SMALLER LAKES. WE WILL THUS BE ABLE TO CORRECT VIMS OBSERVATIONS FOR THE ADJACENCY EFFECT AND LOOK FOR ABSORPTION FEATURES IN THOSE DATA. THIS WORK REPRESENT THE FIRST COMPREHENSIVE MAPPING OF LIQUID ETHANE ON TITAN'S SURFACE THEREBY EXTENDING THE SCIENCE RETURN OF THE CASSINI MISSION. THE RESULTS WILL PROVIDE A USEFUL GUIDE FOR FUTURE MISSIONS INFORMING THE SELECTION OF A SPLASH DOWN SITE FOR LAKE SAMPLERS AND TARGETS FOR LAKE-MONITORING CAMPAIGNS BY AN ORBITER. ETHANE-RICH LAKES MAY BE OF MORE INTEREST AS SITES OF ASTROBIOLOGICAL POTENTIAL GIVEN THEIR LONGEVITY AND HIGHER SOLUBILITY WITH TITAN'S SURFACE ORGANICS.