THE HALO OF THE MILKY WAY IS HOME TO A POPULATION OF GASEOUS HIGH-VELOCITY CLOUDS (HVCS) THAT TRACE THE EXCHANGE OF MATTER BETWEEN THE GALAXY AND ITS SURROUNDINGS. HVCS HAVE BEEN STUDIED EXTENSIVELY VIA H I 21 CM EMISSION AND UV METAL-LINE ABSORPTION. HERE WE PROPOSE A THIRD COMPLEMENTARY APPROACH FOR STUDYING HVCS: SURVEYING THEM IN UV LYMAN SERIES H I ABSORPTION USING ALL AGN SPECTRA IN THE FAR-ULTRAVIOLET SPECTROSCOPIC EXPLORER (FUSE) ARCHIVE. THIS H I SURVEY WILL CONSTITUTE A METAL-INDEPENDENT VIEW OF THE BARYONS IN THE GALACTIC HALO AT A LEVEL OVER 1000 TIMES MORE SENSITIVE THAN 21 CM SURVEYS AND IT CAN BE CONDUCTED WITH ARCHIVAL DATA ALONE. 67 AGN ARE AVAILABLE IN THE FUSE ARCHIVES WITH SUITABLE PROPERTIES (S/N>4 AT 977 A) AND THE DATA ARE REDUCED AND READY FOR ANALYSIS.WITH THESE DATA WE WILL CALCULATE HVC SKY COVERING FRACTIONS IN H I ABSORPTION AND CONDUCT HVC METALLICITY MEASUREMENTS IN SIGHTLINES WITH UV METAL ABSORPTION IN HST/COS OR HST/STIS SPECTRA. WE WILL CALCULATE THE GALACTIC H I COLUMN DENSITY DISTRIBUTION FUNCTION (CDDF) THE INCIDENCE OF H I CLOUDS PER UNIT COLUMN DENSITY THAT ENCODES UNDERLYING DENSITY AND IONIZATION VARIATIONS AND IS SENSITIVE TO THE ESCAPING IONIZATION RADIATION FIELD. THE CDDF HAS BEEN MEASURED AT HIGH REDSHIFTS OVER EIGHT ORDERS OF MAGNITUDE OF H I COLUMN DENSITY VIA QUASAR-ABSORPTION LINE EXPERIMENTS. HOWEVER THE GALACTIC H I CDDF HAS UNTIL NOW ONLY BEEN CONSTRAINED AT HIGH H I COLUMN DENSITY WHERE HVCS CAN BE SEEN IN 21CM EMISSION. OUR DETAILED WORK PLAN WILL INVOLVE IDENTIFYING AND MODELING HVC ABSORPTION IN TEN LYMAN SERIES LINES FROM LY GAMMA 972 TO LY MU 917 IN EACH SIGHT LINE IN THE FUSE SAMPLE. THIS WILL CONSTRAIN THE H I CDDF IN THE COLUMN DENSITY RANGE LOG N(H I)~14 TO 18. BY COMBINING WITH THE EXISTING H I CDDF IN 21 CM HVCS IN THE RANGE LOG N(H I)~18 TO 21 FROM THE ALL-SKY GASS SURVEY WE WILL PRODUCE A GLOBAL GALACTIC CDDF COMPLETE OVER SEVEN ORDERS OF MAGNITUDE PROVIDING KEY NEW INFORMATION ON THE DISTRIBUTION OF DIFFUSE GAS IN THE GALACTIC HALO. THIS WILL ALLOW US TO PLACE THE MILKY WAY S HALO IN THE CONTEXT OF THOSE OF EXTERNAL GALAXIES AND TO IDENTIFY THE GALACTIC CONTRIBUTION FROM BOUND GAS IN HALOS TO THE EXTRAGALACTIC CDDF.