THE VARIETY OF DISCREPANCIES BETWEEN OBSERVATIONS AND SIMULATIONS ON GALACTIC SCALES FROM THE ANISOTROPIC DISTRIBUTION OF DWARF GALAXIES TO THE TOO BIG TO FAIL PROBLEM (WHERE MASSIVE SATELLITES IN SIMULATIONS ARE TOO DENSE RELATIVE TO OBSERVATIONS) SUGGESTS THAT WEMAY NOT YET FULLY UNDERSTAND GALAXY FORMATION. IF THESE SATELLITES EXIST THEY WOULD LEAVE TRACES OF THEIR PASSAGE IN EXTENDED HI DISKS. EXTENDED HI DISKS OF GALAXIES REACH TO SEVERAL TIMES THE OPTICAL RADIUS PRESENTING THE LARGEST POSSIBLE CROSS-SECTION FOR INTERACTION WITHSUB-HALOS AT LARGE DISTANCES (WHERE THEORETICAL MODELS EXPECT THEM TO BE). WE WILL PROVIDE DEFINITIVE CONSTRAINTS ON THE DISTRIBUTION OF DARK MATTER IN SPIRAL GALAXIES BY BUILDING ON OUR ONGOING WORK IN CHARACTERIZING GALACTIC SATELLITES FROM ANALYSIS OF DISTURBANCES INEXTENDED HI DISKS WITH RESPECT TO HYDRODYNAMICAL SIMULATIONS.SPIRAL GALAXIES IN THE LOCAL VOLUME (FROM THE MILKY WAY TO THE XUV DISKS DISCOVERED BY GALEX) EXHIBIT A WEALTH OF UNEXPLAINED MORPHOLOGY BUT THESE MORPHOLOGICAL SIGNATURES HAVE NOT YET BEEN USED TO PLACE CONSTRAINTS ON THE EVOLUTION OF HI DISKS AND THE DARK MATTER DISTRIBUTION. WE ARE NOW POISED TO MAKE SIGNIFICANT PROGRESS IN GALACTOSEISMOLOGY I.E. CONNECT MORPHOLOGICALDISTURBANCES WITH THE MASS DISTRIBUTION. BY USING THE FIRE MODEL FOR EXPLICIT STAR FORMATION AND FEEDBACK WE WILL ALSO DEVELOP A BETTER UNDERSTANDING FOR THE STAR FORMATION HISTORY OF OUR GALAXY AND XUV DISKS.OUR MILKY WAY MODELS WILL BE INFORMED BY THE HST PROPER MOTIONS AND WILL MATCH THE OBSERVED PLANAR DISTURBANCES THE WARP AND VERTICAL WAVES RECENTLY DISCOVERED BY THE RAVE AND LAMOST SURVEYS. WE ARE ALSO CARRYING HIGH RESOLUTION SIMULATIONS WITH THE GIZMO CODE THAT INCORPORATES THE FIRE MODEL TO DEVELOP A COMPREHENSIVE UNDERSTANDING OF THE STAR FORMATION HISTORY ANDSTAR FORMATION RATE (THAT MATCHES SPITZER OBSERVATIONS) OF THE MILKY WAY. THESE MODELS WILL PROVIDE A MUCH NEEDED INTERPRETATIVE FRAMEWORK FOR JWST AND WFIRST OBSERVATIONS.BY MAPPING TO THE HI IMAGE THE GALEX UV IMAGE THE MULTI-WAVELENGTH SED OF XUV DISKS AS WELL AS THE MASSES AND DEPROJECTED DISTANCES OF THE SATELLITES IN A STATISTICALLY ROBUST WAY USING A MONTE CARLO MARKOV CHAIN ANALYSIS WE WILL PRODUCE EVOLUTIONARY HISTORIES OF XUV DISKS AND THEIR SATELLITE POPULATIONS FOR THE FIRST TIME. THIS WILL ENABLE AN APPLES-TO-APPLES COMPARISON FOR XUV DISKS IN THE LOCAL VOLUME. THERE IS CURRENTLY NO STUDY THAT HAS EXAMINED THE MORPHOLOGICAL EFFECTS OF SATELLITES IN COSMOLOGICAL SIMULATIONS ON THE GAS AND STELLAR DISK. THIS IS A CRITICAL TEST OF THE DISTRIBUTION (THE NUMBER THE MASS AND ORBITS) OF SATELLITES IN COSMOLOGICAL SIMULATIONS.WE WILL ALSO INVESTIGATE IF THE VAST POLAR STRUCTURE (VPOS) OF DWARF GALAXIES AROUND THE MILKY WAY IS A SERIOUS PROBLEM FOR THE LAMBDA-CDM PARADIGM. HERE WE ASK TWO SIMPLE QUESTIONS: 1) IS THE VPOS DYNAMICALLY COHERENT? IF THE VPOS IS A SERIOUS PROBLEMFOR CDM ONE EXPECTS THAT IT SHOULD PERSIST OVER A DYNAMICAL TIME AND SHOULD NOT BE UNIQUE TO THE PRESENT DAY. 2) ARE THERE CERTAIN SATELLITES THAT DRIVE THE APPEARANCE OF THE PLANAR STRUCTURE AT PRESENT DAY IF SO IT IS CRITICAL TO EXAMINE WHETHER A SUB-SET EXCLUDINGTHESE SATELLITES RESEMBLES COSMOLOGICAL SIMULATIONS. OUR PRELIMINARY RESULTS SHOW THAT THIS STRUCTURE IS NOT DYNAMICALLY COHERENT AND IS DRIVEN BY TWO SATELLITES: LEO I AND LEO II BOTH OF WHICH HAVE EXTREME KINEMATIC PROPERTIES. WE WILL ALSO EXAMINE THE EVOLUTION OF THEVPOS IN NON- SPHERICAL AND TIME-DEPENDENT POTENTIALS. WE WILL SEEK TO OBTAIN MORE ACCURATE PROPER MOTIONS OF LEO II IN THE UPCOMING HST CYCLE AS WE FIND THAT LEO II PARTICULARLY INFLUENCES THE FIT TO THE PLANAR STRUCTURE.THESE RESULTS WILL HAVE FAR-REACHING IMPACT IN UNDERSTANDING DATA FROM MANY NASA MISSIONS -- HST GALEX SPITZER AND HERSCHEL TO JWST AND WFIRST MISSIONS. WE WILL ALSO PROVIDE A FRAMEWORK FOR UNDERSTANDING DATA FROM THE GAIA AND GALAH SURVEYS OF THE MILKY WAY.