THE PRESENT DAY RESPONSE OF THE MARS AND VENUS UPPER ATMOSPHERES TO THE SOLAR CYCLE VARIATION OF THE SOLAR RADIATION FIELDS [SOLAR WIND AND SOLAR EXTREME ULTRAVIOLET (EUV)] IS THE FOCUS OF THE NEW GENERATION OF MARS AND VENUS MISSIONS BY NASA AND THE EUROPEAN SPACE AGENCY (ESA). THESE MISSIONS ARE MARS EXPRESS (MEX) THE MARS ATMOSPHERE AND VOLATILE EVOLUTION MISSION (MAVEN) AND VENUS EXPRESS (VEX). EACH SPACECRAFT IS EQUIPPED WITH A UV SPECTROMETER [110 TO 360 NM]. THE MOST RECENT MISSION IS MAVEN WITH AN IMAGING ULTRAVIOLET SPECTROGRAPH (IUVS) BUILT BY THE UNIVERSITY OF COLORADO [CU] LABORATORY FOR ATMOSPHERIC AND SPACE PHYSICS (LASP). UV SPECTROSCOPY OF MARS PROVIDES AN IMPORTANT CLUE TO THE PATHWAYS RESPONSIBLE FOR REMOVING GAS (E.G. WATER ESCAPE) FROM THE UPPER ATMOSPHERE TO SPACE OVER EONS. IN THIS PROPOSAL WE WILL UTILIZE THE CU LASP MAVEN-IUVS ENGINEERING MODEL IN THE LABORATORY WHICH OPERATES AT MODERATE SPECTRAL RESOLUTION (~0.5 1.0NM FWHM) TO OBTAIN THE FIRST FULL VIBRATIONAL SPECTRUM IN THE MIDDLE ULTRAVIOLET (MUV) OF THE CAMERON BAND (CB) SYSTEM CO FROM BOTH CO DIRECT EXCIATION AND CO2 DISSOCIATIVE EXCITATION AND SIMILARLY IN THE FUV FOR THE FOURTH POSITIVE BAND SYSTEM OF CO FROM 120-190 NM. THESE BANDS ARE EXCITED IN THE DAYGLOW BY IMPACT OF ELECTRONS FROM 20 TO 200 EV ON BOTH CO AND CO2 PARENT GASES. WE WILL PERFORM LABORATORY MEASUREMENTS BY ELECTRON IMPACT FLUORESCENCE USING MONO-ENERGETIC ELECTRONS TO EXCITE THESE TWO BAND SYSTEMS BY THE SAME PROCESSES AS OCCURS ON MARS (AND ALSO VENUS) BY PHOTOELECTRONS AND AURORAL ELECTRON PRECIPITATION. BY THIS MEANS AS A FIRST STEP WE CAN ASCERTAIN IDENTIFICATION OF THE CB BAND SYSTEM VIBRATIONAL STRUCTURE DETERMINE ROTATIONAL TEMPERATURES AND MEASURE EMISSION CROSS SECTIONS FOR THE STRONGEST ELECTRONIC BAND SYSTEMS ON MARS AND VENUS. THERE ARE PRESENTLY UNCERTAINTIES BY AS MUCH AS A FACTOR OF TWO IN THE EXISTING MEASUREMENTS OF THE CB EMISSION CROSS SECTION FOR ELECTRON IMPACT AFFECTING ACCURATE MODELING ANALYSIS OF ELECTRON TRANSPORT. WE ALSO INDICATE THAT THE MEXP SPICAM (SPECTROSCOPY FOR INVESTIGATION OF CHARACTERISTICS OF THE ATMOSPHERE OF MARS) AND VEXP SPICAV UV DATA ARE NOW PART OF THE PUBLIC RECORD. THE PRIMARY SOURCE OF THE SPICAM SPICAV AND IUVS MUV EMISSIONS ARE THE CB [CO)] FROM 180-260 NM AND CO2+ UV DOUBLET AT 288.3 AND 289.6 NM. IN OUR LAB PROGRAM AT CU WE HAVE OBTAINED THE FIRST CALIBRATED MUV SPECTRA AND EMISSION CROSS SECTION AT 100 EV OF THE OPTICALLY FORBIDDEN CB FROM BOTH CO AND CO2 PARENT GASES FROM EACH PARENT MOLECULE. THE ACCURACY OF THE DETERMINATION OF BASIC DYNAMICAL PROPERTIES WILL BE IMPROVED FOR THE FIRST TIME IN A GENERATION FROM OUR PROPOSED LABORATORY PROGRAM. WE WILL MODEL THE MAVEN SPICAV AND SPICAM OBSERVATIONAL SPECTRA BY THE TECHNIQUE OF MULTIPLE-LINEAR-REGRESSION (MLR) TO FIT THE OBSERVED SPECTRUM USING SPECTRAL VECTORS PREDOMINANTLY ACHIEVED IN THE LABORATORY. FOR THE MEASUREMENT OF THE LABORATORY SPECTRA WE MAKE USE OF THE MAVEN IUVS BREADBOARD INSTRUMENT IN A 2M DIAMETER MOBI VACUUM TANK. THE LARGE CHAMBER IS NECESSARY TO STUDY THE MUV EMISSION FROM THE LONG-LIVED PARENT STATE CO AND IN THE FUV O 5S EMISSION AT 135.5 NM. THIS PROPOSED LABORATORY UV/VISIBLE/IR PROGRAM HAS A MAIN GOAL OF AIDING THE TWO MARS MISSIONS AND ONE VENUS ATMOSPHERIC MISSION PROVIDING TENS OF THOUSANDS OF GLOBAL SCALE ATMOSPHERIC SPECTRA. THIS LABORATORY PROPOSAL SUPPORTS THE NASA SSW GOAL OF IMPROVING OUR UNDERSTANDING OF ATMOSPHERIC PROCESSES IN THE THERMOSPHERE AND IONOSPHERE ON VENUS AND MARS BY PROVIDING FOR ACCURATELY FORWARD MODELING THE DETAILED-BALANCE OF ATMOSPHERIC CONDITIONS REQUIRED TO MATCH WITH THE SPACECRAFT-ACQUIRED LOW-RESOLUTION UV SPECTRA (~0.5 1.0 NM) OF THEIR EMISSION BAND SYSTEMS WITH THE MARS AND VENUS AURIC (ATMOSPHERIC ULTRAVIOLET RADIANCE INTEGRATED CODE) AND OTHER ELECTRON TRANSPORT CODES.