THE RANGE IN STELLAR MASS STAR FORMATION RATE AND METALLICITY IN THESE GALAXIES WILL ALLOW MARGARET TO OBSERVATIONALLY TIE THE HIGH MASS X-RAY BINARY (HMXB} POPULATION TO ITS STAR FORMING ENVIRONMENT. THESE THREE GALAXIES VARY BY OVER TWO ORDERS OF MAGNITUDE IN STELLAR MASS AND MASS-SCALED STAR FORMATION RATE AND RANGE FROM SUB TO SOLAR METALLICITY. WHEN COMPARING TO THEORETICAL PREDICTIONS THIS WILL ALLOW MARGARET TO PROBE THE PHYSICS OF BINARY STELLAR EVOLUTION IN A VARIETY OF STELLAR ENVIRONMENTS. THE PROXIMITY OF THESE THREE GALAXIES MEANS THAT THE STELLAR POPULATIONS CAN BE RESOLVED ALLOWING FOR SPATIALLY RESOLVED STAR FORMATION AND METALLICITY MAPS AND IDENTIFICATION OF INDIVIDUAL COMPANION STARS TO ACCRETING COMPACT OBJECTS IN HMXBS. THE STUDY FOCUSES ON XRBS IN M31 M33 AND THE SMC THAT HAVE BEEN OBSERVED BY NUSTAR CHANDRA AND HUBBLE. THE FOCUS ON HMXBS IS FOR SEVERAL REASONS: 1. HMXBS HAVE COMPANION STARS THAT ARE MASSIVE AND BRIGHT ENOUGH TO BE OBSERVED WITH HUBBLE IN M31 AND M33 AND 2. IN HMXBS BOTH OBJECTS WILL EVENTUALLY BECOME A BH OR NS MAKING THESE SYSTEMS POSSIBLE PRECURSORS TO BINARY BLACK HOLE AND NEUTRON STAR MERGERS OBSERVABLE WITH GRAVITATIONAL WAVES. TO COMPARE THE COMPACT OBJECT {CO} TYPES AND MASSES OF THE COMPANION STARS WITH THEORETICAL PREDICTIONS A SAMPLE FOR WHICH BOTH HIGH QUALITY UV-OPTICAL-LR AND HARD X-RAY OBSERVATIONS ARE AVAILABLE IS REQUIRED.