CLUSTERS BEING THE LARGEST ORGANIZED STRUCTURES IN THE UNIVERSE PROVIDE IMPORTANT CLUES ON HOW BARYON STRUCTURE FORMS AND EVOLVES IN DEEP DARK MATTER POTENTIAL WELLS. ADDITIONALLY THE CLUSTER MASS FUNCTION PROVIDES AN INDEPENDENT TEST FOR COSMOLOGICAL PARAMETERS. UNAC- COUNTED NON-THERMAL PRESSURE SUPPORT (VIA MAJOR MERGERS OR COSMIC ACCRETION) IN CALCULATIONS OF THE CLUSTER MASS FUNCTION A PRIMARY DIAGNOSTIC FOR CLUSTER COSMOLOGY MAY INTRODUCE A BIAS IN COSMOLOGICAL CONSTRAINTS OBTAINED FROM CLUSTERS. TO DATE DUE TO THE TECHNOLOGICAL LIMITATIONS THE DIRECT MEASUREMENTS OF GAS MOTIONS IN THE INTRA-CLUSTER MEDIUM HAVE BEEN LIMITED TO JUST ONE CLUSTER (HITOMI COLLABORATION ET AL. 2018). PREVIOUS INDIRECT MEASURE- MENTS THROUGH SURFACE BRIGHTNESS FLUCTUATIONS AND RESONANT SCATTERING HAVE BEEN LIMITED TO THE CLUSTER CORES (CHURAZOV ET AL. 2012; GASPARI&CHURAZOV 2013; ZHURAVLEVA ET AL. 2015). KHATRI&GASPARI (2016) PROVIDED THE FIRST MILESTONE TO COMBINE DENSITY FLUCTUA- TIONS THROUGH CHANDRA AND XMM-NEWTON X-RAY AND PRESSURE FLUCTUATIONS THROUGH PLANCK SZ MEASUREMENTS TO DETERMINE TURBULENCE IN CLUSTER OUTSKIRTS. WE PROPOSE TO EXTEND THESE MEASUREMENTS TO 60 SOUTH POLE TELESCOPE SELECTED CLUSTERS OBSERVED WITH XMM-NEWTON TO PROVIDE THE MOST STRINGENT CONSTRAINTS ON THE VELOCITY OF GAS MOTIONS AND THE LEVEL OF NON- THERMAL PRESSURE SUPPORT IN CLUSTERS Y TAKING ADVANTAGE OF THE HIGH THROUGHPUT AND LARGE FIELD-OFVIEW OF XMM-NEWTON AND THE (6 ) SMALLER BEAM AND (>2 ) LOWER NOISE OF THE SPT SURVEY RELATIVE TO PLANCK.