A SIGNIFICANT FRACTION OF EXOPLANETS ORBIT WITHIN 0.1 AU OF THEIR HOST STAR WITH PERIODS OF<20 DAYS. THE DISCOVERY OF THESE CLOSEIN PLANETS HAS DEFIED CONVENTIONAL MODELS OF PLANET FORMATION AND EVOLUTION BASED ON OUR OWN SOLAR SYSTEM. IT IS WIDELY ACCEPTED THAT THESE CLOSE-IN PLANETS DID NOT FORM IN SUCH CLOSE PROXIMITY TO THEIR HOST STARS (BOTH ROCKY PLANETS AND HOT JUPITERS) BUT RATHER THAT DYNAMICAL OR INTERACTIVE PROCESSES CAUSED THEM TO MIGRATE INWARDS FROM LARGER ORBITAL SEMIMAJOR AXES AND PERIODS. THERE ARE MULTIPLE PLANET MIGRATION SCENARIOS PROPOSED IN THE LITERATURE THOUGH IT IS UNCLEAR HOW MUCH OF THE KNOWN PLANET POPULATION IS ATTRIBUTABLE TO EACH MECHANISM. PLANETARY MIGRATION MODELS CAN BE LOOSELY DIVIDED INTO TWO CATEGORIES: DISK-DRIVEN MIGRATION AND DYNAMICAL MIGRATION. DISK MIGRATION OCCURS OVER THE LIFETIME OF THE PROTOPLANETARY DISK (<5 MYR) WHILE MIGRATION INVOLVING DYNAMICAL MULTI-BODY INTERACTIONS OPERATES ON TIMESCALES OF ~100 MYR TO ~1GYR A LENGTHIER PROCESS THAN DISK MIGRATION. THE K2 MISSION HAS MEASURED PLANET FORMATION TIMESCALES AND MIGRATION PATHWAYS BY SAMPLING GROUPS OF STARS AT KEY AGES. OVER THE PAST 10 CAMPAIGNS MULTIPLE GROUPS OF YOUNG STARS HAVE BEEN OBSERVED BY K2 RANGING FROM THE 10 MYR UPPER SCORPIUS OB ASSOCIATION THROUGH THE ~120 MYR PLEIADES CLUSTER TO THE ~600-800 MYR HYADES AND PRAESEPE CLUSTERS. UPCOMING DATA FROM MORE RECENT CAMPAIGNS INCLUDE THE 2MYR TAURUS REGION AND SIGNIFICANTLY MORE UPPER SCORPIUS MEMBERS IN C13 AND 15. THE FREQUENCY ORBITAL PROPERTIES AND COMPOSITIONS OF THE EXOPLANET POPULATION IN THESE SAMPLES OF DIFFERENT AGE WITH CAREFUL TREATMENT OF DETECTION COMPLETENESS DISTINGUISH THESE SCENARIOS OF EXOPLANET MIGRATION AS THEIR HOST STARS ARE SETTLING ONTO THE MAIN SEQUENCE. WE HAVE PIONEERED EFFORTS TO IDENTIFY TRANSITING EXOPLANETS IN THE K2 DATA FOR YOUNG CLUSTERS AND MOVING GROUPS AND HAVE DEVELOPED A NEW HIGHLY COMPLETE DETRENDING ALGORITHM FOR ROTATIONAL INDUCED VARIABILITY THAT IS COMMONLY SEEN IN THE LIGHT CURVES OF YOUNG ACTIVE STARS (RIZZUTO ET AL. IN PREP). WE HAVE IDENTIFIED 11 CANDIDATE PLANETS IN PRAESEPE HYADES UPPER SCO AND THE PLEIADES USING THESE METHODS THE FIRST OF WHICH HAS NOW BEEN PUBLISHED WITH FOLLOW-UP (MANN ET AL. 2016ABC; GAIDOS ET AL. 2016). THIS SAMPLE OF DETECTED PLANET CANDIDATES GIVES A PROMISING FIRST INDICATION OF THE TIMESCALE OVER WHICH PLANET MIGRATION OCCURS FAVORING DYNAMICAL MULTI-BODY PROCESSES. HOWEVER BECAUSE ROTATIONAL ACTIVITY IN YOUNG STARS MAKES DETECTION OF EXOPLANET TRANSITS MORE DIFFICULT FOR THE YOUNGER CLUSTERS (E.G UPPER SCO PLEIADES) TO ROBUSTLY PROVE THAT THESE FREQUENCIES ARE TRUE REPRESENTATIONS OF THE SHORT-PERIOD PLANET OCCURRENCE RATE AT DIFFERENT PMS AGES WILL REQUIRE ROBUST DETERMINATION OF DETECTION LIMITS IN THESE HIGHLY VARIABLE YOUNG-STAR LIGHTCURVES. WE PROPOSE TO ADDRESS THE QUESTION OF PLANET MIGRATION WITH A UNIFORM INJECTION-RECOVERY TEST OF YOUNG CLUSTER MEMBERS TO ROBUSTLY MEASURE THE DETECTABILITY OF PLANETS OF DIFFERING SIZE AND ORBIT. THIS WILL INVOLVE DETRENDING THE LIGHT CURVE DATA OF INSTRUMENTAL AND ROTATIONAL SYSTEMATICS INJECTING A SYNTHETIC TRANSIT SIGNATURE FROM A GRID OF PLANETARY AND ORBITAL PARAMETERS REVERSING THE DETRENDING AND THEN EXECUTING OUR TRANSIT SEARCH PIPELINE (WHICH IS TUNED FOR HIGHLY ACTIVE YOUNG STARS) AND MAPPING THE RECOVERY RATE AS A FUNCTION OF PLANET PARAMETERS FOR EVERY INDIVIDUAL LIGHT CURVE. WITH THIS MAP OF DETECTABILITY AS A FUNCTION OF PLANET PROPERTIES FOR EACH LIGHT CURVE AND A FULL PROGRAM OF DETECTED EXOPLANET FOLLOW-UP WE CAN THEN DIRECTLY CONFIRM ANY CHANGE IN THE OCCURRENCE RATES OF CLOSE-IN (P<20 DAY) PLANETS WITH CLUSTER AGE AND IDENTIFY THE MOST SIGNIFICANT MIGRATION MECHANISM.