THE COSMIC OPTICAL BACKGROUND (COB) IS THE SUMMED EMISSION FROM ALL SOURCES OUTSIDE OF OUR GALAXY EMITTED AT WAVELENGTHS CORRESPONDING TO THOSE VISIBLE WITH THE HUMAN EYE. THE COB IS A POWERFUL DIAGNOSTIC OF THE EMISSION FROM KNOWN ASTROPHYSICAL PROCESSES IN GALAXIES INCLUDING STELLAR NUCLEOSYNTHESIS MASS ACCRETION ONTO BLACK HOLES AND THE GRAVITATIONAL COLLAPSE OF STARS SO IS CRUCIAL IN UNDERSTANDING THE TOTAL EMISSION FROM STARS IN THE UNIVERSE. FURTHER COMPARISON OF THE COB INTENSITY TO THE SURFACE BRIGHTNESS ARISING FROM KNOWN GALAXY POPULATIONS CAN REVEAL THE PRESENCE OF DIFFUSE BACKGROUNDS PRODUCED BY MORE EXOTIC PHENOMENA SUCH AS THE DECAY OF PARTICLE SPECIES OUTSIDE THE STANDARD MODEL OR LIGHT FROM OBJECTS OUTSIDE OF GALAXIES. DESPITE A GREAT DEAL OF INTEREST DIRECT PHOTOMETRIC MEASUREMENT OF THE COB HAS PROVEN TO BE CHALLENGING. THE EARTH'S ATMOSPHERE IS SEVERAL ORDERS OF MAGNITUDE BRIGHTER THAN THE COB AND SUNLIGHT SCATTERED FROM INTERPLANETARY DUST (IPD) PARTICLES IN THE SOLAR SYSTEM PRODUCES A SIMILARLY LARGE FOREGROUND. ACCOUNTING FOR THE RELEVANT EMISSION ABSORPTION AND SCATTERING EFFECTS IN EITHER SOURCE IS A DAUNTING TASK. IT IS THUS DESIRABLE TO MEASURE THE COB FROM VANTAGE POINTS WHERE THE EARTH'S ATMOSPHERE AND THE LIGHT FROM IPD ARE NOT APPRECIABLE COMPONENTS OF THE DIFFUSE SKY BRIGHTNESS SUCH AS THE OUTER SOLAR SYSTEM.NASA'S NEW HORIZONS (NH) MISSION HAS GIVEN US AN UNPRECEDENTED VIEW OF AND FROM THE OUTER REACHES OF THE SOLAR SYSTEM. IN ADDITION TO THEIR PLANETARY IMAGING FUNCTIONS SOME OF THE NH INSTRUMENTS CAN DOUBLE AS SENSITIVE ASTRONOMICAL TELESCOPES WORKING AT OPTICAL AND NEAR-IR WAVELENGTHS. OUR TEAM HAS ALREADY ANALYZED DATA FROM THE LONG RANGE RECONNAISSANCE IMAGER (LORRI) INSTRUMENT ACQUIRED DURING NH'S CRUISE PHASE TO MEASURE THE COB IN A SINGLE WIDE BANDPASS (ZEMCOV ET AL. 2017 NATURE COMMUNICATIONS). IN THAT WORK WE PLACED A 2 SIGMA STATISTICAL UPPER LIMIT ON THE COB BRIGHTNESS OF<19 NW M^-2 SR^-1 A LEVEL ABOUT TWICE AS LARGE AS THE SUMMED LIGHT FROM GALAXIES. THE MEASUREMENT IS FROM ONLY 260S OF INTEGRATION TIME USING A DATA SET WITH CHARACTERISTICS THAT COMPLICATE ASTROPHYSICAL EXAMINATION; WE CONCLUDE THAT ADDITIONAL NH DATA COULD SIGNIFICANTLY IMPROVE THIS LIMIT. IN THIS NFDAP PROGRAM WE PROPOSE TO USE ARCHIVAL NH DATA TO MEASURE THE COSMIC OPTICAL BACKGROUND AND SEARCH FOR DIFFUSE LIGHT ASSOCIATED WITH INTERPLANETARY DUST IN BOTH THE INNER AND OUTER SOLAR SYSTEM. TO IMPROVE ON OUR PREVIOUS MEASUREMENT WE WILL USE PUBLICLY AVAILABLE DATA FROM THE LORRI NAVIGATION CAMPAIGNS AND PLUTO FLYBY AS WELL AS NEAR-IR DATA FROM THE RALPH INSTRUMENT TO EXPAND THE STUDY'S WAVELENGTH COVERAGE. THE PDS ARCHIVE CURRENTLY CONTAINS OVER 15 000 S OF EXPOSURES TAKEN DURING THESE PHASES OF THE MISSION OF WHICH WE EXPECT ~6% TO BE USEFUL FOR THIS STUDY. THIS REPRESENTS A FACTOR OF 3.5 INCREASE IN INTEGRATION TIME OVER OUR INITIAL STUDY BUT WITH DIFFERENT SYSTEMATIC ERRORS LEADING TO AT LEAST A SIGNAL TO NOISE RATIO 3 MEASUREMENT OF THE INTEGRATED LIGHT FROM GALAXIES. TO MEASURE THE COB WE WILL USE METHODS SIMILAR TO THOSE IN OUR PREVIOUS WORK WHERE ASSESSMENTS OF THE SURFACE BRIGHTNESS FROM STARS DIFFUSE GALACTIC LIGHT DARK CURRENT IN THE DETECTOR AND OTHER EMISSION SOURCES ARE SUBTRACTED FROM THE MEAN OF EACH IMAGE TO MEASURE THE SURFACE BRIGHTNESS RESIDUAL. WE WILL CONSTRAIN THE VARIATION IN THE BRIGHTNESS OF THE DIFFUSE GALACTIC LIGHT BY COMPARING MEASUREMENTS OF THE DIFFUSE BACKGROUND WITH THERMAL IR EMISSION AND SEARCHING FOR CORRELATIONS. FINALLY WE WILL SEARCH FOR LIGHT REFLECTED FROM THE IPD CLOUD BY SEARCHING FOR DIFFUSE BANDS OF LIGHT ALONG THE ECLIPTIC. OUR TEAM HAS A PROVEN TRACK RECORD ANALYZING THESE TYPE OF MEASUREMENTS AND WITH THE WEALTH OF NH DATA THAT IS CURRENTLY AVAILABLE WE EXPECT TO DETECT THE COB WITH WELL-UNDERSTOOD SYSTEMATIC ERRORS FOR THE FIRST TIME.