MEASUREMENTS OF INTRACLUSTER GAS PROPERTIES TO LARGE RADII WHERE MOST OF THE CLUSTER MASS (AND VOLUME) RESIDES ARE IMPORTANT FORA DETAILED UNDERSTANDING OF THE PHYSICS OF THE INTRACLUSTER MEDIUM (ICM) WHICH IS IN MANY RESPECTS STILL POORLY UNDERSTOOD AND ISREQUIRED FOR THE USE OF CLUSTERS AS COSMOLOGICAL PROBES. THE SUZAKU X-RAY OBSERVATORY HAS ALLOWED FOR THE FIRST TIME MEASUREMENTSOF THE INTRACLUSTER MEDIUM (ICM) GAS OUT TO THE VIRIAL RADII OF CLUSTERS. SUCH STUDIES HAVE GENERALLY FOUND ICM ENTROPY PROFILES THATFALL BELOW THE EXPECTED SELF-SIMILAR RELATION BASED ON PURELY GRAVITATIONAL COLLAPSE ("ENTROPY FLATTENING") AND BARYON FRACTIONS THATEXCEED THE COSMIC VALUE NEAR THE VIRIAL RADII OF CLUSTERS. PROPOSED EXPLANATIONS INCLUDE THE PRESENCE OF COOL UNRESOLVED GAS CLUMPS;WEAKENING ACCRETION SHOCKS; AND ELECTRON-ION NON-EQUILIBRIUM. THESE MECHANISMS ARE EXPECTED TO CORRELATE WITH LARGE SCALE STRUCTURE WITH A GREATER EFFECT IN THE DIRECTIONS OF LARGE SCALE FILAMENTS. PREVIOUS STUDIES HAVE SHOWN THAT ENTROPY FLATTENING IN CLUSTER OUTSKIRTSDEPENDS ON AZIMUTH BUT HAVE BEEN UNABLE TO CORRELATE THIS EFFECT WITH LARGE SCALE STRUCTURE.TO DISENTANGLE THE DEPENDENCE ON LARGE SCALE STRUCTURE WE PERFORMED 360 KS MOSAIC SUZAKU OBSERVATIONS OF THE STRONGLY MERGINGCLUSTER ABELL 98 (A98). THIS SYSTEM IS IN A PRE MERGER STATE WITH TWO CLEARLY SEPARATED ROUGHLY EQUAL MASS SUBCLUSTERS. SUCHMAJOR BINARY MERGERS ARE EXPECTED TO TAKE PLACE ALONG LARGE SCALE STRUCTURE FILAMENTS. A THIRD SUBCLUSTER ALONG THE SAME LINE (INPROJECTION) FURTHER SUGGESTS THE PRESENCE OF A LARGE SCALE STRUCTURE FILAMENT. IT IS ONE OF THE BEST EXAMPLES OF A TRIPLE CLUSTER ALONG ALARGE SCALE FILAMENT. WE HAVE PERFORMED SUZAKU OBSERVATIONS OUT TO THE VIRIAL RADIUS IN THIS SYSTEM IN TWO DIRECTIONS BOTH ALONG ANDPERPENDICULAR TO THE MERGER AXIS (AND HENCE THE PUTATIVE LARGE SCALE FILAMENT). A DETAILED SPECTROSCOPIC ANALYSIS OF THE ICM WILL REVEALWHETHER ENTROPY FLATTENING CORRELATES WITH LARGE SCALE STRUCTURE AS SUGGESTED BY THE CURRENT LEADING "GAS CLUMPING" MODEL OR WHETHEROTHER MODELS ARE MORE LIKELY. WE ALSO SEARCH FOR THE DENSE END OF THE WARM-HOT INTERGALACTIC MEDIUM (WHIM) WHICH TRACES LARGESCALE FILAMENTS AND IS THOUGHT TO CONTAIN THE BULK OF THE "MISSING BARYONS" AT LOW REDSHIFT. WE NOTE THAT DESPITE THE POTENTIAL POWERFOR BINARY PRE-MERGER SYSTEMS LIKE A98 TO DISCRIMINATE BETWEEN PROPOSED MECHANISMS FORENTROPY PROFILE FLATTENING IN CLUSTER OUTSKIRTS(DUE TO THE A PRIORI KNOWLEDGE OF THE EXISTENCE AND ORIENTATION OF THE LOCAL LARGE SCALE FILAMENT) SUCH STUDIES ARE VERY RARE. THUS THEWORK WE PROPOSE HERE REPRESENTS A SIGNIFICANT CONTRIBUTION TO OUR UNDERSTANDING OF SUCH SYSTEMS.DETAILED ANALYSIS OF THE FAINT EXTENDED EMISSION IN CLUSTER OUTSKIRTS IS VERY CHALLENGING AND REQUIRES DETAILED MODELING OF THEBACKGROUND AND SYSTEMATIC UNCERTAINTIES. THE FUNDING WE PROPOSE FOR HERE WILL SUPPORT THE DATA ANALYSIS OF AND PUBLICATION OF RESULTSFROM OUR SUZAKU OBSERVATIONS OF A98 (WHICH HAVE BEEN PUBLIC SINCE ACQUISITION SINCE THIS PROJECT IS A SUZAKU "LARGE PROJECT"). THISSTUDY WILL CONTRIBUTE TO NASA'S STRATEGIC OBJECTIVE TO "DISCOVER HOW THE UNIVERSE WORKS EXPLORE HOW IT BEGAN AND EVOLVED AND SEARCHFOR LIFE ON PLANETS AROUND OTHER STARS" BY ADDRESSING THE ASSOCIATED SCIENCE GOAL OF "[EXPLORING] THE ORIGIN AND EVOLUTION OF THE GALAXIES STARS AND PLANETS THAT MAKE UP OUR UNIVERSE."