5 THE MILKY WAY HAS A HOT HALO OF GAS AT LEAST TENS OF KPC IN SIZE, PROBABLY EXTENDING TO THE VIRIAL RADIUS, IF NOT BEYOND. INITIAL STUDIES OF THE HOT HALO PROPERTIES SHOW THAT OPTICAL DEPTH EFFECTS ARE IMPORTANT FOR THE O VII AND O VIII LINES, WHICH DOMINATE THE X RAY EMISSION AND ABSORPTION PROPERTIES. TO ACCOUNT FOR OPTICAL DEPTH EFFECTS, WE WILL USE A MONTE CARLO RADIATIVE TRANSFER CODE IN CONJUNCTION WITH A PARAMETRIC DENSITY MODEL TO OBTAIN A BEST FIT FOR THE EXISTING O VII AND O VIII EMISSION AND ABSORPTION LINE DATA. WITH THE RICH ARCHIVAL DATA SET, WE WILL OBTAIN DEFINING VALUES FOR THE DENSITY AND PRESSURE PROFILES, THE GAS MASS AS A FUNCTION OF RADIUS, THE METALLICITY, AND THE MEAN DOPPLER B PARAMETER. EXPANDING INTO THIS HOT HALO ARE THE FERMI BUBBLES, LARGE STRUCTURES THAT EXTEND 8 KPC ABOVE AND BELOW THE GALACTIC CENTER AND ARE FILLED WITH COSMIC RAYS. THE FERMI BUBBLES ARE PRODUCED BY EITHER A STARBURST EVENT OR AGN ACTIVITY FROM SGR A. THEY ARE PROBABLY EXPANDING SUPERSONICALLY INTO THE HOT HALO, PROVIDING SIGNIFICANT HEATING, BUT TO OBTAIN ACCURATE VALUES FOR OF THE SHOCK STRENGTHS AND MAGNITUDE OF THIS FEEDBACK, WE NEED TO ISOLATE THE INTERACTION LAYER. WE WILL ACCOMPLISH THIS BY SUBTRACTING THE HOT HALO MODEL AND MAKING THE NECESSARY OPTICAL DEPTH CORRECTIONS TO THE X RAY OBSERVATIONS. THE OBSERVATIONS WILL ALSO DETERMINE WHETHER HOT THERMAL GAS LIES WITHIN THE BUBBLE. FINALLY, WE WILL SEARCH FOR ANALOGS TO THE FERMI BUBBLES IN EXTRAGALACTIC EDGE ON SPIRAL GALAXIES. THIS ANALYSIS WILL CONSTRAIN THE AGN DUTY CYCLE AND ENERGY INPUT, DETERMINING THE IMPORTANCE OF AGN FEEDBACK IN LOW REDSHIFT GALACTIC EVOLUTION. THE BEST SIGNATURE IS THE HARD X RAY EMISSION PRODUCED THROUGH INVERSE COMPTON SCATTERING, AND THERE IS ALREADY A SUGGESTION OF A DETECTION. Other Administrative Action $0 2/3/20 Not listed THE MILKY WAY HAS A HOT HALO OF GAS AT LEAST TENS OF KPC IN SIZE PROBABLY EXTENDING TO THE VIRIAL RADIUS IF NOT BEYOND. INITIAL STUDIES OF THE HOT HALO PROPERTIES SHOW THAT OPTICAL DEPTH EFFECTS ARE IMPORTANT FOR THE O VII AND O VIII LINES WHICH DOMINATE THE X RAY EMISSION AND ABSORPTION PROPERTIES. TO ACCOUNT FOR OPTICAL DEPTH EFFECTS WE WILL USE A MONTE CARLO RADIATIVE TRANSFERCODE IN CONJUNCTION WITH A PARAMETRIC DENSITY MODEL TO OBTAIN A BEST FIT FOR THE EXISTING O VII AND O VIII EMISSION AND ABSORPTION LINE DATA. WITH THE RICH ARCHIVAL DATA SET WE WILL OBTAIN DEFINING VALUES FOR THE DENSITY AND PRESSURE PROFILES THE GAS MASS AS A FUNCTION OF RADIUS THE METALLICITY AND THE MEAN DOPPLER B PARAMETER. EXPANDING INTO THIS HOT HALO ARE THE FERMI BUBBLES LARGESTRUCTURES THAT EXTEND 8 KPC ABOVE AND BELOW THE GALACTIC CENTER AND ARE FILLED WITH COSMIC RAYS. THE FERMI BUBBLES ARE PRODUCED BY EITHER A STARBURST EVENT OR AGN ACTIVITY FROM SGR A. THEY ARE PROBABLY EXPANDING SUPERSONICALLY INTO THE HOT HALO PROVIDING SIGNIFICANT HEATING BUT TO OBTAIN ACCURATE VALUES FOR OF THE SHOCK STRENGTHS AND MAGNITUDE OF THIS FEEDBACK WE NEED TO ISOLATE THE INTERACTION LAYER. WE WILL ACCOMPLISH THIS BY SUBTRACTING THE HOT HALO MODEL AND MAKING THE NECESSARY OPTICAL DEPTH CORRECTIONS TO THE X RAY OBSERVATIONS. THE OBSERVATIONS WILL ALSO DETERMINE WHETHER HOT THERMAL GAS LIES WITHIN THE BUBBLE. FINALLY WE WILL SEARCH FOR ANALOGS TO THE FERMI BUBBLES IN EXTRAGALACTIC EDGE ON SPIRAL GALAXIES. THIS ANALYSIS WILL CONSTRAIN THE AGN DUTY CYCLE AND ENERGY INPUT DETERMINING THE IMPORTANCE OF AGN FEEDBACK IN LOW REDSHIFT GALACTIC EVOLUTION. THE BEST SIGNATURE IS THE HARD X RAY EMISSION PRODUCED THROUGH INVERSE COMPTON SCATTERING AND THERE IS ALREADY A SUGGESTION OF A DETECTION. $0 2/3/20 4 THE MILKY WAY HAS A HOT HALO OF GAS AT LEAST TENS OF KPC IN SIZE, PROBABLY EXTENDING TO THE VIRIAL RADIUS, IF NOT BEYOND. INITIAL STUDIES OF THE HOT HALO PROPERTIES SHOW THAT OPTICAL DEPTH EFFECTS ARE IMPORTANT FOR THE O VII AND O VIII LINES, WHICH DOMINATE THE X RAY EMISSION AND ABSORPTION PROPERTIES. TO ACCOUNT FOR OPTICAL DEPTH EFFECTS, WE WILL USE A MONTE CARLO RADIATIVE TRANSFER CODE IN CONJUNCTION WITH A PARAMETRIC DENSITY MODEL TO OBTAIN A BEST FIT FOR THE EXISTING O VII AND O VIII EMISSION AND ABSORPTION LINE DATA. WITH THE RICH ARCHIVAL DATA SET, WE WILL OBTAIN DEFINING VALUES FOR THE DENSITY AND PRESSURE PROFILES, THE GAS MASS AS A FUNCTION OF RADIUS, THE METALLICITY, AND THE MEAN DOPPLER B PARAMETER. EXPANDING INTO THIS HOT HALO ARE THE FERMI BUBBLES, LARGE STRUCTURES THAT EXTEND 8 KPC ABOVE AND BELOW THE GALACTIC CENTER AND ARE FILLED WITH COSMIC RAYS. THE FERMI BUBBLES ARE PRODUCED BY EITHER A STARBURST EVENT OR AGN ACTIVITY FROM SGR A. THEY ARE PROBABLY EXPANDING SUPERSONICALLY INTO THE HOT HALO, PROVIDING SIGNIFICANT HEATING, BUT TO OBTAIN ACCURATE VALUES FOR OF THE SHOCK STRENGTHS AND MAGNITUDE OF THIS FEEDBACK, WE NEED TO ISOLATE THE INTERACTION LAYER. WE WILL ACCOMPLISH THIS BY SUBTRACTING THE HOT HALO MODEL AND MAKING THE NECESSARY OPTICAL DEPTH CORRECTIONS TO THE X RAY OBSERVATIONS. THE OBSERVATIONS WILL ALSO DETERMINE WHETHER HOT THERMAL GAS LIES WITHIN THE BUBBLE. FINALLY, WE WILL SEARCH FOR ANALOGS TO THE FERMI BUBBLES IN EXTRAGALACTIC EDGE ON SPIRAL GALAXIES. THIS ANALYSIS WILL CONSTRAIN THE AGN DUTY CYCLE AND ENERGY INPUT, DETERMINING THE IMPORTANCE OF AGN FEEDBACK IN LOW REDSHIFT GALACTIC EVOLUTION. THE BEST SIGNATURE IS THE HARD X RAY EMISSION PRODUCED THROUGH INVERSE COMPTON SCATTERING, AND THERE IS ALREADY A SUGGESTION OF A DETECTION. Other Administrative Action $0 2/8/19 Not listed THE MILKY WAY HAS A HOT HALO OF GAS AT LEAST TENS OF KPC IN SIZE PROBABLY EXTENDING TO THE VIRIAL RADIUS IF NOT BEYOND. INITIAL STUDIES OF THE HOT HALO PROPERTIES SHOW THAT OPTICAL DEPTH EFFECTS ARE IMPORTANT FOR THE O VII AND O VIII LINES WHICH DOMINATE THE X RAY EMISSION AND ABSORPTION PROPERTIES. TO ACCOUNT FOR OPTICAL DEPTH EFFECTS WE WILL USE A MONTE CARLO RADIATIVE TRANSFERCODE IN CONJUNCTION WITH A PARAMETRIC DENSITY MODEL TO OBTAIN A BEST FIT FOR THE EXISTING O VII AND O VIII EMISSION AND ABSORPTION LINE DATA. WITH THE RICH ARCHIVAL DATA SET WE WILL OBTAIN DEFINING VALUES FOR THE DENSITY AND PRESSURE PROFILES THE GAS MASS AS A FUNCTION OF RADIUS THE METALLICITY AND THE MEAN DOPPLER B PARAMETER. EXPANDING INTO THIS HOT HALO ARE THE FERMI BUBBLES LARGESTRUCTURES THAT EXTEND 8 KPC ABOVE AND BELOW THE GALACTIC CENTER AND ARE FILLED WITH COSMIC RAYS. THE FERMI BUBBLES ARE PRODUCED BY EITHER A STARBURST EVENT OR AGN ACTIVITY FROM SGR A. THEY ARE PROBABLY EXPANDING SUPERSONICALLY INTO THE HOT HALO PROVIDING SIGNIFICANT HEATING BUT TO OBTAIN ACCURATE VALUES FOR OF THE SHOCK STRENGTHS AND MAGNITUDE OF THIS FEEDBACK WE NEED TO ISOLATE THE INTERACTION LAYER. WE WILL ACCOMPLISH THIS BY SUBTRACTING THE HOT HALO MODEL AND MAKING THE NECESSARY OPTICAL DEPTH CORRECTIONS TO THE X RAY OBSERVATIONS. THE OBSERVATIONS WILL ALSO DETERMINE WHETHER HOT THERMAL GAS LIES WITHIN THE BUBBLE. FINALLY WE WILL SEARCH FOR ANALOGS TO THE FERMI BUBBLES IN EXTRAGALACTIC EDGE ON SPIRAL GALAXIES. THIS ANALYSIS WILL CONSTRAIN THE AGN DUTY CYCLE AND ENERGY INPUT DETERMINING THE IMPORTANCE OF AGN FEEDBACK IN LOW REDSHIFT GALACTIC EVOLUTION. THE BEST SIGNATURE IS THE HARD X RAY EMISSION PRODUCED THROUGH INVERSE COMPTON SCATTERING AND THERE IS ALREADY A SUGGESTION OF A DETECTION. $0 2/8/19 Not listed THE MILKY WAY HAS A HOT HALO OF GAS AT LEAST TENS OF KPC IN SIZE PROBABLY EXTENDING TO THE VIRIAL RADIUS IF NOT BEYOND. INITIAL STUDIES OF THE HOT HALO PROPERTIES SHOW THAT OPTICAL DEPTH EFFECTS ARE IMPORTANT FOR THE O VII AND O VIII LINES WHICH DOMINATE THE X RAY EMISSION AND ABSORPTION PROPERTIES. TO ACCOUNT FOR OPTICAL DEPTH EFFECTS WE WILL USE A MONTE CARLO RADIATIVE TRANSFERCODE IN CONJUNCTION WITH A PARAMETRIC DENSITY MODEL TO OBTAIN A BEST FIT FOR THE EXISTING O VII AND O VIII EMISSION AND ABSORPTION LINE DATA. WITH THE RICH ARCHIVAL DATA SET WE WILL OBTAIN DEFINING VALUES FOR THE DENSITY AND PRESSURE PROFILES THE GAS MASS AS A FUNCTION OF RADIUS THE METALLICITY AND THE MEAN DOPPLER B PARAMETER. EXPANDING INTO THIS HOT HALO ARE THE FERMI BUBBLES LARGESTRUCTURES THAT EXTEND 8 KPC ABOVE AND BELOW THE GALACTIC CENTER AND ARE FILLED WITH COSMIC RAYS. THE FERMI BUBBLES ARE PRODUCED BY EITHER A STARBURST EVENT OR AGN ACTIVITY FROM SGR A. THEY ARE PROBABLY EXPANDING SUPERSONICALLY INTO THE HOT HALO PROVIDING SIGNIFICANT HEATING BUT TO OBTAIN ACCURATE VALUES FOR OF THE SHOCK STRENGTHS AND MAGNITUDE OF THIS FEEDBACK WE NEED TO ISOLATE THE INTERACTION LAYER. WE WILL ACCOMPLISH THIS BY SUBTRACTING THE HOT HALO MODEL AND MAKING THE NECESSARY OPTICAL DEPTH CORRECTIONS TO THE X RAY OBSERVATIONS. THE OBSERVATIONS WILL ALSO DETERMINE WHETHER HOT THERMAL GAS LIES WITHIN THE BUBBLE. FINALLY WE WILL SEARCH FOR ANALOGS TO THE FERMI BUBBLES IN EXTRAGALACTIC EDGE ON SPIRAL GALAXIES. THIS ANALYSIS WILL CONSTRAIN THE AGN DUTY CYCLE AND ENERGY INPUT DETERMINING THE IMPORTANCE OF AGN FEEDBACK IN LOW REDSHIFT GALACTIC EVOLUTION. THE BEST SIGNATURE IS THE HARD X RAY EMISSION PRODUCED THROUGH INVERSE COMPTON SCATTERING AND THERE IS ALREADY A SUGGESTION OF A DETECTION. $147.2k 5/21/18