A NUMBER OF NASA MISSIONS PLAN TO USE NEW MEMS TECHNOLOGY TO ENABLE MULTI-OBJECT SPECTROSCOPY CAPABILITIES IN SPACE. FOR EXAMPLE, THE PROPOSED SMALL SATELLITE ISCEA (INFRARED SMALLSAT FOR CLUSTER EVOLUTION ASTROPHYSICS) AND THE PROBE CLASS MISSION ATLAS (ASTROPHYSICS TELESCOPE FOR LARGE AREA SPECTROSCOPY) PLAN TO UTILIZE DMDS AS A RAPIDLY RE-CONFIGURABLE SLIT MASK ARRAY TO ENABLE MULTI-OBJECT SPECTROSCOPY. DMD-BASED MULTI-OBJECT SPECTROGRAPHS (MOS) ARE BECOMING A MATURE CONCEPT, WITH SEVERAL INSTRUMENTS BEING CONSTRUCTED FOR 4 M AND 6 M TELESCOPES. A DMD MOS IS ESPECIALLY INTERESTING FOR SPACE APPLICATIONS, BECAUSE OF ITS EXTREME FLEXIBILITY. IN ADDITION TO TRUE MULTI-OBJECT SPECTROSCOPY, WITH HUNDREDS OF SLITLETS PLACED ACROSS THE FIELD OF VIEW, THESE INSTRUMENTS CAN ALSO OPERATE AS INTEGRAL FIELD SPECTROGRAPHS, USING THE HADAMARD TRANSFORM SPECTRAL IMAGING (HTSI) TECHNIQUE. HTSI IS BASED ON THE HADAMARD TRANSFORM TECHNIQUE, WHICH OFFERS THE HIGHEST IMPROVEMENT IN SIGNAL-TO-NOISE (SNR) IN RECONSTRUCTED SIGNALS OF ANY OPTICAL MULTIPLEXING TECHNIQUE. THE IMPROVEMENT IN SNR ENABLES INCREASED MEASUREMENT EFFICIENCY AS COMPARED TO TRADITIONAL SINGLE SLIT SPECTROSCOPY TECHNIQUES. HTSI IMPLEMENTS THIS TECHNIQUE THROUGH TWO-DIMENSIONAL SPATIAL MULTIPLEXING AND PRODUCES SPATIALLY RESOLVED SPECTRA. AN HTSI OBSERVING MODE CAN BE IMPLEMENTED ON EXISTING AND PROPOSED DMD-BASED MOS WITH NO CHANGES TO THE HARDWARE OR DESIGN. THE ADDITION OF THIS OBSERVING MODE CAN INCREASE THE UTILITY OF THESE INSTRUMENTS BY ADDING THE CAPABILITY OF MEASURING SPATIALLY RESOLVED SPECTRA IN AN EFFICIENT MANNER. WITH THE HTSI OBSERVING MODE, A SERIES OF N DMD MASK PATTERNS ARE GENERATED FROM THE ROWS OF A HADAMARD MATRIX WITH AN ORDER OF N AND USED TO CAPTURE N IMAGES (OR IMAGE PAIRS). IMAGES CAPTURED BY THE SPECTROGRAPH S DETECTOR CONSIST OF ONE AXIS OF PURE SPATIAL INFORMATION AND A SECOND AXIS WITH CONVOLVED SPECTRAL AND SPATIAL INFORMATION DUE TO SPECTRAL OVERLAP. THE SERIES OF N IMAGES FORM AN OUTPUT DATA CUBE WHERE THE THIRD AXIS REPRESENTS THE DMD MASK NUMBER (I.E. ROW OF THE HADAMARD MATRIX). THE INVERSE HADAMARD TRANSFORM IS APPLIED TO THIS DATA CUBE TO DE-CONVOLVE SPECTRAL AND SPATIAL INFORMATION AND RECONSTRUCT THE ORIGINAL SIGNALS FROM THE SKY. THE FINAL PRODUCT IS A DATA CUBE WITH TWO DIMENSIONS OF SPATIAL INFORMATION AND ONE DIMENSION OF SPECTRAL INFORMATION. THE IMPROVEMENT IN SNR FOR HTSI MEASUREMENTS IS UP TO A FACTOR OF .N/2 IN COMPARISON TO THE SAME VOLUME OF DATA CAPTURED WITH TRADITIONAL SINGLE-SLIT METHODS. THE MAXIMUM IMPROVEMENT IN SNR IS REALIZED WHEN DETECTOR NOISE DOMINATES, AS IS OFTEN THE CASE FOR FAINT SPECTRAL SIGNALS. HOWEVER, THIS IMPROVEMENT IN SNR CAN ALSO BE LIMITED BY NOISE AND ERRORS IN THE MULTIPLEXED MEASUREMENTS. SUCCESSFUL IMPLEMENTATION OF THE TECHNIQUE WITH EXISTING AND PLANNED DMD-BASED MOS REQUIRES A THOROUGH EVALUATION OF THE IMPACT OF VARIOUS SOURCES OF NOISE AND ERRORS THAT MAY ARISE IN ASTRONOMICAL OBSERVATIONS. THIS PROJECT SEEKS TO FURTHER DEVELOP THE HTSI TECHNIQUE FOR USE IN ASTRONOMY APPLICATIONS. THE DEVELOPMENT WORK WILL INCLUDE COMPUTER MODELING, LABORATORY MEASUREMENTS, AND IMPLEMENTATION OF AN HTSI OBSERVING MODE WITH THE GROUND-BASED INSTRUMENT SAMOS. THIS WORK AIMS TO PROVIDE A THOROUGH INVESTIGATION OF THE TECHNIQUE'S LIMITATIONS AND SUCCESS RELATIVE TO ASTRONOMY APPLICATIONS. IT WILL PAVE THE WAY FOR FUTURE DMD-BASED MOS TO SUCCESSFULLY IMPLEMENT THE HTSI OBSERVING MODE, ADDING THE UNIQUE CAPABILITY OF BEING ABLE TO QUICKLY SWITCH BETWEEN MULTI-OBJECT AND INTEGRAL FIELD SPECTROSCOPY MEASUREMENTS.