HOT GASEOUS HALOS AROUND GALAXIES ARE A KEY COMPONENT THAT AROSE FROM THE FORMATION AND EVOLUTION OF THESE SYSTEMS. THE X-RAY EMISSION FROM THIS GAS MAINLY PROBES THE INNER REGION (WITHIN 20 KPC) AND THIS EMISSION IS FITTED WITH RADIAL SURFACE PROFILES AND SPECTRAL MODELS TO INFER THE SPATIAL DISTRIBUTION OF THE DENSITY TEMPERATURE AND METALLICITY. SUCH ANALYSIS HAS IGNORED RADIATIVE TRANSFER EFFECTS EVEN THOUGH WE KNOW THAT THE OPTICAL DEPTH CAN REACH 10 IN SOME LINES. WE PROPOSE ANALYSIS OF THESE DATA WITH MODELS THAT INCLUDE A MONTE CARLO RADIATIVE TRANSFER TREATMENT; MOST DATA WILL BE FROM XMM-NEWTON AND SUZAKU. THESE CALCULATIONS MAY LEAD TO SIGNIFICANT CHANGES IN THE BASIC PROPERTIES OF THE GAS WHICH IN TURN AFFECTS THE INTERPRETATION FOR THE ORIGIN AND EVOLUTION OF THE GAS. WE WILL MAKE MODEL AVAILABLE BY INCORPORATING IT INTO THE XSPEC SUITE OF MODELS. THE SECOND LARGER EFFORT INVOLVES INVESTIGATIONS INTO THE HOT GAS CONTENT OF GALAXIES AND GALAXY GROUPS FROM THE PLANCK SUNYAEV- ZELDOVICH (SZ) SIGNAL. THIS SIGNAL MEASURES THE PRODUCT OF THE GAS MASS AND THE MEAN TEMPERATURE SO IT MAINLY COMES FROM HOT GAS NEAR THE VIRIAL TEMPERATURE AND EXTENDING TO THE VIRIAL RADIUS (MUCH LARGER THAN THE X-RAY EMISSION REGION). FROM EXISTING SZ MAPS WE SHOW THAT SOME INDIVIDUAL NEARBY GALAXIES AND GROUPS SHOULD BE DETECTABLE AND FROM INITIAL WORK WE INDEED DETECT EXTENDED SZ SIGNALS FROM SOME L* GALAXIES (E.G. M81; TYPICALLY TO 100-200 KPC) FROM NEARBY GALAXY GROUPS AND FROM MORE DISTANT HIGH-MASS GALAXIES OFTEN IMBEDDED IN GROUPS OR CLUSTERS. THESE REMARKABLE DETECTIONS DEMAND A THOROUGH ANALYSIS OF THE NOISE PROPERTIES AND FOREGROUND/BACKGROUND CONTAMINATION THAT CAN AFFECT THE RESULTS AND WE PROPOSE TO CONDUCT SUCH AN ANALYSIS. THEN IN ONE PROGRAM WE WILL QUANTIFY THE SZ SIGNAL FROM LOCAL GALAXIES NEAR L* (DISTANCES<15 MPC) WHERE WE APPEAR TO HAVE 8 DETECTIONS ABOVE 3SIGMA AND A NUMBER OF OTHERS JUST BELOW. THESE MEASUREMENTS YIELD THE HOT GAS MASS WHICH APPEARS TO BE A SIGNIFICANT FRACTION OF THE MISSING BARYONS. A SECOND PROGRAM WILL DETERMINE THE DISTRIBUTION OF HOT GAS MASSES IN NEARBY GALAXY GROUPS. THIS WILL IDENTIFY GROUPS THAT ARE TRUE BOUND SYSTEMS AND ARE VIRIALIZED IN A MASS RANGE WHERE THE SCALING RELATIONSHIPS APPEAR TO BREAK DOWN. IN THE THIRD PROJECT WE INVESTIGATE WHETHER THE PUBLISHED STACKING RESULTS OF MASSIVE GALAXIES LEAD TO REPRESENTATIVE MEASURES OF THEIR HOT GAS MASS AS THERE IS CURRENTLY A SIGNIFICANT DISCREPANCY. FOR A SAMPLE OF MASSIVE GALAXIES WHERE MSTAR = 2-3E11 MSUN WE WILL DETERMINE THE UNDERLYING DISTRIBUTION OF THE SZ SIGNAL WHICH HAS NEVER BEEN DONE. PRELIMINARY WORK OF A SAMPLE OF THE NEAREST OBJECTS USED IN STACKING SHOWS THAT MOST ARE INDIVIDUALLY DETECTED WITH SEVERAL HAVING LARGE SZ SIGNALS FROM THE SURROUNDING GROUP OR CLUSTER IN WHICH THEY LIE. THE PROPOSED STUDY MAY SHOW THAT THE DISTRIBUTION OF THE SZ SIGNAL IS SO BROAD THAT CALCULATING A MEAN SZ SIGNAL AS A FUNCTION OF GALAXY STELLAR MASS IS TOO SIMPLISTIC AND CAN PRODUCE MISLEADING INTERPRETATIONS.