THE HOT GAS IN GALAXY HALOS AS THE MOST EXTENDED AND VOLUME FILLING PHASE OF THE CIRCUM-GALACTIC MEDIUM (CGM) TYPICALLY DISTRIBUTED BEYOND THE GALACTIC DISK AND BULGE AND WITHIN THE VIRIAL RADIUS OF THEIR DARK MATTER HALOS PLAYS A KEY ROLE IN THE CO-EVOLUTION OF GALAXIES AND THEIR ENVIRONMENT. DURING ALMOST TWO DECADES OF OPERATION XMM-NEWTON HAS COLLECTED A RICH ARCHIVE OF SOFT X-RAY OBSERVATIONS OF NEARBY GALAXY HALOS. HOWEVER ALTHOUGH BEING THE MOST SENSITIVE X-RAY TELESCOPE MOST OF THESE XMM-NEWTON OBSERVATIONS TOWARD INDIVIDUAL GALAXIES ARE STILL NOT DEEP ENOUGH FOR THE STUDY OF THE EXTENDED HOT CGM TO A SIGNIFICANT FRACTION OF THE VIRIAL RADIUS OF THE DARK MATTER HALO. WE HAVE DEVELOPED TOOLS FOR STACKING ANALYSIS AND ADOPTED THEM TO A SMALL SAMPLE OF NEARBY MASSIVE SPIRAL GALAXIES EACH OBSERVED WITH A MODERATELY DEEP XMM-NEWTON EXPOSURE. THIS PRELIMINARY WORK HAS ACHIEVED A DETECTION OF THE HOT CGM TO A RADIAL RANGE AT LEAST TWICE AS FAR AWAY AS THE EXISTING WORKS BASED ON DEEP X-RAY OBSERVATIONS OF INDIVIDUAL GALAXIES OR STACKING ANALYSIS WITH ROSAT DATA. WE CAN THEN BETTER CONSTRAIN THE RADIAL DISTRIBUTION OF THE HOT CGM AND ESTIMATE THE BARYON MASS CONTAINED IN IT. THE RESULTS HAVE STRONG CONSTRAINT ON MODELS PREDICTING THE RADIAL DISTRIBUTION OF THE HOT CGM AND FURTHER HAVE IMPORTANT SCIENTIFIC IMPLICATIONS ON SOME WIDELY DEBATED PROBLEMS SUCH AS THE MISSING BARYON PROBLEM. WE HEREIN PROPOSE TO EXPAND THIS ANALYSIS TO THE ENTIRE XMM-NEWTON ARCHIVE OF MORE THAN 1000 NEARBY GALAXIES TO STUDY THE RADIAL DISTRIBUTION OF HOT CGM AROUND VARIOUS TYPES OF GALAXIES. WE WILL STUDY THE FOLLOWING SPECIFIC SCIENTIFIC PROBLEMS: (1) WE WILL STACK THE XMM-NEWTON DATA OF EACH SUBSAMPLE IN ORDER TO DETECT THE EXTENDED HOT CGM BEYOND THE INNER HALO HIGHLY DISTURBED BY GALACTIC FEEDBACK. BASED ON THIS STACKING ANALYSIS WE WILL EXAMINE IF OR NOT THE RADIAL DISTRIBUTION OF HOT GAS PROPERTIES AT LARGE RADII CAN BE CHARACTERIZED WITH ANY UNIVERSAL SELF-SIMILAR RELATIONS WHICH HAVE BEEN ADOPTED TO MORE MASSIVE SYSTEMS SUCH AS GALAXY GROUPS OR CLUSTERS. (2) WE WILL FURTHER ESTIMATE THE TOTAL MASS CONTAINED IN THIS HOT CGM AND COMPARE THE BARYON BUDGET AND ITS INTRINSIC SCATTER OF THE GALAXIES IN DIFFERENT MASS RANGE OR WITH DIFFERENT STAR FORMATION AND ENVIRONMENTAL PROPERTIES. (3) WE WILL MEASURE THE RADIATIVE COOLING RATE OF THE HALO GAS AND EXAMINE IF IT CAN BE A POTENTIALLY IMPORTANT SOURCE OF GAS SUPPLY TO CONTINUE STAR FORMATION. (4) WE WILL SEARCH FOR THE EXTENDED HARD X-RAY CONTINUUM AND FE K LINE EMISSIONS IN SOME CAREFULLY SELECTED GALAXY SAMPLES IN ORDER TO ESTIMATE THE COSMIC RAY AND THERMAL PRESSURES AND STUDY THEY ROLE IN DRIVING GALACTIC OUTFLOWS. IN ADDITION TO THE ABOVE SPECIFIC SCIENTIFIC GOALS WE WILL ALSO CONSTRUCT A CATALOGUE OF BOTH POINT-LIKE AND EXTENDED X-RAY SOURCES WHICH WILL BE THE FIRST CATALOGUE OF EXTENDED X-RAY SOURCES WITH DEEP X-RAY IMAGES AND UNIFORMLY DEFINED MORPHOLOGICAL PARAMETERS. THE ABOVE ANALYSIS SCIENTIFIC DISCUSSIONS AND ONLINE CATALOGUE WILL HELP US TO NOT ONLY BETTER UNDERSTAND THE ROLE OF THE HOT CGM IN THE CO-EVOLUTION OF GALAXIES AND THEIR ENVIRONMENT BUT ALSO HAVE A BETTER TECHNICAL JUSTIFICATION AND PROSPECT ON THE SCIENTIFIC ACHIEVEMENT OF THE NEXT GENERATION X-RAY TELESCOPES.