CARBONACEOUS CHONDRITES ARE NATURALLY DELIVERED SAMPLES FROM ASTEROID PARENT BODIES. LINKING THESE METEORITES TO ASTEROIDS AND MORE FUNDAMENTALLY UNDERSTANDING THE CAUSES OF OBSERVED VARIATIONS IN ASTEROID SPECTRAL PROPERTIES REQUIRES UNDERSTANDING HOW SPECTRAL ATTRIBUTES ARE AFFECTED BY THE PRESENCE AND ABSENCE OR PREVALENCE OF PHASES (MINERAL MINERALOID AND VOLATILE) AND CHEMICAL INDICATORS OF ALTERATION. STUDIES OF MOST- AND LEAST-ALTERED CARBONACEOUS CHONDRITES SHOW VARIATIONS IN THE PRESENCE/ABSENCE OF A 0.7 M ABSORPTION DUE TO IRON IN PHYLLOSILICATES 1.0-1.5 M ABSORPTIONS DUE TO MAFIC MINERALS 2.7-3.0 M ABSORPTIONS DUE TO OH/H2O AND SILICATE FEATURES FROM 8-12 M. SIMILARLY TELESCOPIC AND SPACECRAFT SPECTRAL DATA OF PRIMITIVE ASTEROIDS SHOW THESE ABSORPTIONS ARE PRESENT. THEY ARE USED TO CLASSIFY AND UNDERSTAND PROCESSES AFFECTING PRIMITIVE SOLAR SYSTEM BODIES; THERE IS ALSO SUBSTANTIAL LESS UNDERSTOOD SPECTRAL DIVERSITY IN ABSORPTION FEATURES FROM 2.5-4.5 M ATTRIBUTED TO METAL-OH NH3 CARBONATE AND POSSIBLY ORGANICS AND WATER ICE. SPECTROSCOPIC WORK WITH METEORITES TO LINK WITH THE ASTEROIDS HAS TO DATE FOCUSED ON THE SPECTRAL PROPERTIES OF GROUND BULK POWDERS THE PREPARATION OF WHICH HAS DESTROYED OR HOMOGENIZED ANY PRE-EXISTING HETEROGENEITY. HERE WE WILL USE MICROIMAGING REFLECTANCE SPECTROSCOPY TO CHARACTERIZE NOT ONLY THE BULK PROPERTIES OF CARBONACEOUS CHONDRITE SAMPLES BUT ALSO TO EXAMINE THE HETEROGENEITY OF CHONDRITE AND MATRIX MINERAL ASSEMBLAGES RECOGNIZING SMALL (HUNDREDS OF MICRONS TO MM) ZONES OF SPECTRALLY DISTINCT MATERIALS. OUR STUDY WILL FOCUS ON A SUBSET OF KEY PRIMITIVE MATERIALS PRESENTLY POSTULATED TO BE THE MOST DIRECTLY RELATED TO PRIMITIVE ASTEROIDS AND CARBONACEOUS MISSION-TARGET ASTEROIDS (CERES BENNU RYUGU) SPECIFICALLY C1 UNGROUPED C2 CM2 CR AND CV SAMPLES. C-CHONDRITE CLASTS OF DIVERSE DEGREES OF ALTERATION ARE KNOWN TO OCCUR IN BRECCIATED NONCARBONACEOUS METEORITES AND IN CARBONACEOUS CHONDRITES. WE WILL IDENTIFY AND PROVIDE SPATIALLY RESOLVED MAPS OF ABSORPTION BAND DEPTHS AND BAND POSITIONS FOCUSING ON ALL VARIABILITY WITH SPECIAL ATTENTION TO THAT ALSO OBSERVED IN THE ASTEROIDS. WE WILL FOCUS ON CHARACTERIZATION OF MATRIX CLASTS AND CHONDRULES IDENTIFYING AND MAPPING HETEROGENEOUS SPECTRAL CLASSES AND IDENTIFYING SPECIFIC MINERAL PHASES VIA FOLLOW-ON MICROPROBE ANALYSES TO UNDERSTAND AT PIXEL TO SUBPIXEL SCALES THE CONSTITUENTS RESPONSIBLE FOR OBSERVED SPECTRAL VARIABILITY. THIS STUDY EXAMINES THE RESULTS OF EARLY THERMAL AND CHEMICAL PROCESSES OCCURRING ON SMALL BODIES TO UNDERSTAND THE ORIGIN OF METEORITES LINK THESE TO ASTEROID COMPOSITIONAL GROUPS. WE HYPOTHESIZE THAT THIS STUDY MAY REFUTE OR CONFORM TO AND EXTEND CORRELATIONS BETWEEN SOME CHEMICAL INDICES OF ALTERATION AND VISIBLE AND INFRARED FEATURES (TAKIR ET AL. 2013; MCADAM ET AL. 2015) CONFIRMING OR REFUTING THE HYPOTHESIZED SPECIES RESPONSIBLE. ALTERNATIVELY OR ADDITIONALLY THIS STUDY WILL REVEAL WHETHER OBSERVED DIFFERENCES IN SPECTRAL PROPERTIES AND AQUEOUS-ALTERATION METRICS IN C-CHONDRITES ARE THE RESULT OF (A) MIXING IN DIFFERENT PROPORTIONS OF CLASTS FROM MULTIPLE SOURCE REGIONS OR PARENT BODIES WITH DIVERSE PRE-ASSEMBLY ALTERATION STATES OR (B) DIFFERENT DEGREES OF HOMOGENIZING ALTERATION ON THE PARENT BODY(IES) OF THE POST-ASSEMBLY CHONDRITIC BRECCIAS. SUCH MAY ALLOW THE RECOGNITION OF CERES- OR 52 EUROPA-LIKE SPECTRAL CLASSES WITHIN THE EXISTING METEORITE COLLECTION. BY DETERMINING THE LINKAGES BETWEEN SPECTRAL PROPERTIES AND PHASES RESPONSIBLE WE WILL ENABLE IMPROVED INTERPRETATION OF TELESCOPIC AND SPACECRAFT DATA FROM PRIMITIVE BODIES.