WE PROPOSE A STUDY OF THE EVOLUTION OF STELLAR POPULATIONS AND GAS METALLICITIES IN ABOUT 80 NEARBY STAR FORMING GALAXIES BASED ON MINING THE NASA DATA ARCHIVES FOR OBSERVATIONS OF THE [NIII] 57 M [OIII] 52 M AND/OR 88 M [NII] 122 AND [CII] 158 M FARINFRARED (FIR) FINE-STRUCTURE LINES AND OTHER ARCHIVES FOR THERMAL RADIO CONTINUUM. THESE LINES ARE POWERFUL PROBES OF BOTH STELLAR POPULATIONS AND GAS PROPERTIES AND OUR PRIMARY SCIENCE DERIVES FROM THESE TRACERS. FOR SOURCES THAT SHOW BOTH SIGNS OF ACTIVE GALACTIC NUCLEI (AGN) AND STAR FORMATION WE WILL TAKE ADVANTAGE OF THE READILY AVAILABLE NASA SPITZER IRS DATA BASE THAT INCLUDES MID-IR [NEII] 12.8 M [NEIII] 15.6 M AND [NEV] 14.3 M [OIV] 25.9 M AND PAH OBSERVATIONS. THESE COMPLEMENTARY DATA REVEAL THE RELATIVE FRACTIONS OF THE FIR LINE EMISSION THAT MIGHT ARISE FROM STAR FORMATION AND THE NARROW LINE REGIONS (NLR) ASSOCIATED WITH AN AGN THEREBY PROVIDING A ROBUST SET OF OBSERVATIONS TO COMPARE WITH STAR FORMATION MODELS. SUBSETS OF THE FIR LINES HAVE BEEN DETECTED FROM HUNDREDS OF NEARBY GALAXIES. FROM BOTH THEORETICAL STUDIES AND THE RESULTS OF THESE PIONEERING OBSERVATIONS WE KNOW THAT THESE LINES CAN BE POWERFUL PROBES OF STELLAR POPULATIONS AND STAR FORMATION IN GALAXIES. HERE WE PLAN TO USE VARIOUS COMBINATIONS OF THE LINES TO CONSTRAIN (1) THE AGE OF THE STELLAR POPULATIONS (THROUGH LINES THAT TRACE THE HARDNESS OF THE STELLAR RADIATION FIELDS HENCE STELLAR SPECTRAL TYPE) (2) THE DEGREE OF PROCESSING OF THE INTERSTELLAR MEDIUM (THROUGH LINES THAT TRACE GROWTH OF SECONDARY TO PRIMARY ELEMENT ABUNDANCES FOR EXAMPLE THE N/O RATIO) (3) THE EFFICIENCY OF STAR FORMATION (THROUGH GROWTH IN ABSOLUTE ABUNDANCES OF N AND O THE N/H AND O/H RATIOS) AND (4) THE CURRENT DAY MASS FUNCTION OF UPPER MAIN SEQUENCE STARS. SURPRISINGLY THERE HAS BEEN NO SYSTEMATIC STUDY OF THE LARGE SAMPLE OF THESE LINE DETECTIONS MADE WITH PACS ON HERSCHEL IN ORDER TO TRULY ASSESS AND CALIBRATE THEIR DIAGNOSTIC POWER. THE RICH HERSCHEL/PACS DATA SET IS PARTICULARLY ATTRACTIVE FOR THIS STUDY DUE TO ITS SENSITIVITY AND CALIBRATION UNIFORMITY. WE PROPOSE TO UNDERTAKE SUCH A STUDY HERE. AN INITIAL SEARCH OF THE HERSCHEL ARCHIVE REVEALS THAT THERE ARE AT LEAST 80 GALAXIES THAT HAVE BEEN OBSERVED IN THE [NII] 122 M [OIII] 52 AND/OR 88 M AND THE [CII] 158 M LINE. THE PRIMARY GOAL OF THIS PROPOSAL IS TO USE THESE EMISSION LINES TO STUDY THE STAR FORMATION PROPERTIES (AGE METALLICITY INITIAL MASS FUNCTION (IMF) AND STAR FORMATION EFFICIENCY) IN GALAXIES IN THE LOCAL UNIVERSE. THIS LINE OF STUDY TIES INTO OUR OVERARCHING RESEARCH OBJECTIVE WHICH IS TO UNDERSTAND THE EVOLUTION OF STAR AND GALAXY FORMATION OVER COSMIC TIME. WE HAVE BEGUN STUDYING STAR FORMATION IN THE EARLY UNIVERSE BY DETECTING THESE LINES AT HIGH REDSHIFTS WITH OUR GRATING SPECTROMETER ZEUS-2 ON THE APEX TELESCOPE AND THROUGH ALMA PROGRAMS. THE STUDY WE PROPOSE HERE WILL ALLOW US TO CONFIDENTLY APPLY THESE SPECTRAL PROBES TO STUDIES OF HIGH-Z GALAXIES WHILE ALSO PROVIDING NEW INSIGHTS INTO THE CHARACTERISTIC AND PROCESS OF STAR-FORMATION OF GALAXIES IN THE NEARBY UNIVERSE. WE WILL UTILIZE NASA S SPACE ASTROPHYSICS ARCHIVES TO EXPLORE THE EVOLUTION OF STELLAR POPULATIONS AND THE ELEMENTS OVER COSMIC TIME. THE PROPOSED WORK IS THEREFORE HIGHLY RELEVANT TO NASA S STRATEGIC GOAL 1: EXPAND THE FRONTIERS OF KNOWLEDGE CAPABILITY AND OPPORTUNITY IN SPACE. OBJECTIVE 1.6 DISCOVER HOW THE UNIVERSE WORKS EXPLORE HOW IT BEGAN AND EVOLVED AND SEARCH FOR LIFE ON PLANETS AROUND OTHER STARS. SINCE THE PROGRAM INVOLVES BOTH GRADUATE AND UNDERGRADUATE STUDENTS AT A RESEARCH UNIVERSITY WE ALSO ADDRESS STRATEGIC GOAL 2 VIA OBJECTIVE 2.4: ADVANCE THE NATION S STEM EDUCATION AND WORKFORCE PIPELINE BY WORKING COLLABORATIVE WITH OTHER AGENCIES TO ENGAGE STUDENTS TEACHERS AND FACULTY IN NASA S MISSIONS AND UNIQUE ASSETS.