ANALYSIS OF STAR FORMING REGIONS IN A HIGHLY MAGNIFIED LENSED GALAXY AT Z=2.48WE PROPOSE TO MEASURE THE PROPERTIES OF INDIVIDUAL STAR FORMING REGIONS IN A HIGHLY MAGNIFIED GALAXY AT Z=2.48. THE GALAXY IS STRONGLY LENSED BY A GALAXY CLUSTER AT Z=0.659 SDSSJ1110+64 FORMING A GIANT ARC COMPOSED OF THREE MULTIPLE IMAGES OF THE SAME SOURCE GALAXY. DUE TO THE HIGH MAGNIFICATION INDIVIDUAL STAR FORMING REGIONS ARE RESOLVABLE IN OUR HUBBLE SPACE TELESCOPE DATA (G0-13003). WE HAVE COMPUTED AN ACCURATE LENS MODEL FOR SDSSJ1110 AND USE THIS LENS MODEL TO FORM A SOURCE PLANE RECONSTRUCTION OF THE LENSED GALAXY. IMPLYING INNOVATIVE FORWARD-MODELING TECHNIQUES WE WERE ABLE FOR THE FIRST TIME TO MEASURE THE SIZES OF INDIVIDUAL STAR FORMING REGIONS AT SCALES OF TENS OF PARSECS. A PAPER DESCRIBING THE ANALYSIS AND RESULTS IS IN PREPARATION. THE WORK PROPOSED FOR HERE BUILDS UP ON THE PREVIOUS RESEARCH AND WILL EXTEND OUR ANALYSIS OF THE PHYSICAL PROPERTIES OF THE STAR FORMING REGIONS TO ANSWER THE FOLLOWING QUESTIONS: 1) WHAT IS THE STAR FORMATION RATE (SFR) AS A FUNCTION OF THE SIZE OF EACH STARFORMING REGION? IS THERE AN EVOLUTION IN THE SFR SURFACE DENSITY? STUDIES OF STAR FORMING REGIONS IN LOCAL UNIVERSE AND AT HIGH REDSHIFT SUGGEST THAT THE SFR IS CORRELATED WITH THE SIZE OF THE STAR FORMING REGION (HEREAFTER CLUMP) AND THAT IT MONOTONOUSLY INCREASING WITH CLUMP SIZE (E.G. LIVERMORE ET AL. 2016 AND REFERENCES THEREIN); MOREOVER THE NORMALIZATION OF THAT RELATION INCREASES WITH REDSHIFT WHERE HIGHER SFR IS MEASURED AT HIGHER REDSHIFTS. INTERESTINGLY MEASUREMENTS OF THE SFR IN CLUMPS SMALLER THAN 100 PC DO NOT EXIST BEYOND Z=1.5 BECAUSE THEY CANNOT BE RESOLVED WITH CURRENT FACILITIES. THE SUGGESTED WORK WILL FILL IN A VOID IN THE PARAMETER SPACE OF SMALL CLUMPS AT HIGH REDSHIFT WHICH IS ONLY POSSIBLE WITH GRAVITATIONAL LENSING AND HST RESOLUTION. 2) CAN WE INFORM STUDIES OF GALAXIES IN THE FIELD (I.E. NOT LENSED) THAT LACK THE CAPABILITY TO RESOLVE INDIVIDUAL STAR FORMING REGIONS? IN THE FIELD WHAT WOULD WE KNOW ABOUT WHERE STARS FORM? THE GRAVITATIONAL LENSING MAGNIFICATION EFFECTIVELY INCREASES THE TELESCOPE RESOLUTION BY A FACTOR OF 10-30. BY DEGRADING THE SOURCE PLANE RECONSTRUCTED IMAGE OF THE LENSED GALAXY TO THE RESOLUTION OF SURVEYS LIKE CANDELS WE CAN FIND OUT WHAT FRACTION OF THE CLUMPY SFR IS RECOVERED BY THESE STUDIES HOW MUCH OF THE SFR HAPPENS ON SMALL SCALES AND HOW MUCH OF IT IS WRONGLY ASSIGNED TO A DIFFUSE GALAXY-WIDE MODE OF STAR FORMATION.