THE AIM OF THIS PROPOSAL IS TO MEASURE H3+ IONS IN SATURN S MAGNETOSPHERE USING CASSINI CAPS DATA MAP MAGNETOSPHERIC REGIONS WHERE H3+ IS FOUND AND DETERMINE WHETHER THE PRESENCE OF H3+ IN THE MAGNETOSPHERE VARIES WITH TIME. H3+ IN THE MAGNETOSPHERE PRIMARILY COMES FROM SATURN'S IONOSPHERE THEREFORE THE PRESENCE OF H3+ IONS IN A PARTICULAR MAGNETOSPHERIC REGION IS LIKELY TO INDICATE THAT PLASMA IS OUTFLOWING FROM THE REGION OF SATURN'S IONOSPHERE THAT IS MAGNETICALLY-CONNECTED TO THAT MAGNETOSPHERIC REGION. PREVIOUS WORK HAS ESTABLISHED THAT CASSINI CAPS CAN MEASURE THE H3+ COUNT RATE WHICH CAN BE INTERPRETED AS A PROXY FOR H3+ LOCAL DENSITY. WE WILL USE THE SPATIAL DISTRIBUTION OF H3+ IN THE MAGNETOSPHERE TO DETERMINE THE IONOSPHERIC REGIONS FROM WHICH OUTFLOW OCCURS. WE WILL USE TEMPORAL VARIATIONS IN H3+ IN THE MAGNETOSPHERE SUPPORTED BY KNOWLEDGE OF THE SOLAR WIND CONDITIONS AND AURORAL ACTIVITY TO CHARACTERISE THE RELATIONSHIP BETWEEN H3+ OUTFLOWS AND SOLAR WIND FORCING. IONOSPHERIC OUTFLOW IS AN IMPORTANT PROCESS AT EARTH BUT STILL POORLY-CHARACTERISED AT SATURN AND ITS PARAMETERISATION IS A CRITICAL STEP FOR THE UNDERSTANDING THE COUPLING BETWEEN THE PLANET AND ITS SURROUNDING MAGNETOSPHERE. FIRSTLY WE WILL OBTAIN A SPATIAL MAP OF THE DISTRIBUTION OF H3+ IN THE MAGNETOSPHERE WHICH WILL ALSO PROVIDE A PRELIMINARY ESTIMATE OF WHERE THE OUTFLOW REGIONS IN THE IONOSPHERE ARE LOCATED IN RESPECT TO THE AURORAL OVAL IN BOTH HEMISPHERES. THE STANDARD FITTING PROCEDURE FOR CASSINI/CAPS/IMS/TOF/ST MEASUREMENTS YIELDS COUNT RATES FOR DIFFERENT CHARGED SPECIES. HOWEVER IN ORDER TO MEASURE THE H3+ COUNT RATE WE NEED TO REMOVE AN INSTRUMENTAL ARTEFACT THAT COVERS THE H3+ SIGNAL. WE WILL DO THIS BY ADDING A CALIBRATION FUNCTION FOR H3+ TO THE ESTABLISHED STANDARD FITTING PROCEDURE. WE WILL USE THIS UPDATED FITTING PROCEDURE TO FIT ALL AVAILABLE DATA (2004 TO 2012) AND OBTAIN COUNT RATES FOR H3+ AND OTHER SPECIES. ALSO WE WILL USE CASSINI MAG DATA AND CASSINI CAPS/IMS POINTING INFORMATION TO CLASSIFY EACH H3+ COUNT RATE VALUE AS "FIELD-ALIGNED" OR "NOT FIELD-ALIGNED". IN ORDER TO MATCH THE LOCATION OF H3+ MEASUREMENTS TO THEIR IONOSPHERIC SOURCE REGIONS WE WILL USE ONLY MEASUREMENTS CLASSIFIED AS FIELD-ALIGNED . BASED ON ANALOGY WITH EARTH S IONOSPHERIC POLAR OUTFLOW WE ANTICIPATE THAT THE STRONGEST IONOSPHERIC OUTFLOW REGIONS WILL BE LOCATED AT HIGH LATITUDES RATHER THAN AT MID-LATITUDES OR EQUATORIAL LATITUDES. SECONDLY WE WILL CHARACTERISE THE RELATIONSHIP BETWEEN H3+ OUTFLOWS AND SOLAR WIND FORCING. WE WILL USE THE ENLIL MODEL TO DETERMINE UPSTREAM SOLAR WIND CONDITIONS. MOREOVER WE WILL UTILISE ULTRAVIOLET (UV) AND INFRARED (IR) AURORAL DATA - FROM CASSINI/ UVIS HST CAMPAIGNS AND GROUND BASED OBSERVATIONS (IR) - TO DETERMINE THE LEVEL OF AURORAL ACTIVITY. WE WILL COMPARE OUR CAPS H3+ OBSERVATIONS TO THESE SOLAR WIND AND AURORAL OBSERVATIONS TO ASSESS WHICH CONDITIONS ENHANCE H3+ OUTFLOW. THIRDLY WE WILL USE A MAGNETIC FIELD MODEL TO PRECISELY DETERMINE THE IONOSPHERIC OUTFLOW REGIONS ASSOCIATED WITH EACH MAGNETOSPHERIC REGION WHERE H3+ IS PRESENT. THIS WILL CONSTRAIN LATITUDES OF THE OUTFLOW REGIONS. FINALLY WE WILL SYNTHESISE THE RESULTS FROM ALL THREE PHASES OF THIS PROJECT CHARACTERISING THE CONDITIONS UNDER WHICH IONOSPHERIC WIND OUTFLOW OCCURS AND UNDER WHICH IT IS ENHANCED. THIS IS CRUCIAL FOR ATMOSPHERIC AND MAGNETOSPHERE-IONOSPHERE COUPLING MODELS. THIS PROPOSAL ADDRESSES THE MAIN OBJECTIVE OF CDAP TO "ENHANCE THE SCIENTIFIC RETURN OF THE CASSINI MISSION" AND THE DATA WE WILL USE WOULD "INCLUDE BOTH UN-CALIBRATED AND CALIBRATED DATA AS WELL AS HIGHER-ORDER DATA PRODUCTS PRODUCED FROM THE MISSION DATA". AS THE FIRST COMPREHENSIVE SURVEY OF H3+ A KEY IONOSPHERIC TRACER IN SATURN'S MAGNETOSPHERE THIS WORK WOULD MAKE SUBSTANTIAL CONTRIBUTIONS TO UNDERSTANDING THE IONOSPHERIC OUTFLOW PROCESS WHICH IS A CRITICAL ASPECT OF IONOSPHERE-MAGNETOSPHERE COUPLING AT SATURN.