1) TARGET SELECTION AND CHARACTERIZATION - FOLLOWING OUR SUCCESSFUL TARGET PROPOSALS IN K2 FIELDS 0 5 OUR FIELD 6&7 TARGETS ARE DRAWN FROM THE SUPERBLINK PROPER MOTION DATABASE (SB LEPINE&SHARA 2005) AND THE PANSTARRS-1 SURVEY (PS1 KAISER ET AL. 2002). WE USE REDUCED PROPER-MOTION AND OPTICAL/NIR COLOR-CUTS AND SED FITTING. IN SB WE SELECT ALL TARGETS WITH (V J)>2.5 V + 5 LOG + 5<10 AND (6V 7J 3)<5 LOG WHERE IS THE PROPER MOTION. THESE SELECTION CRITERIA CAPTURE THE MAJORITY OF M DWARFS (>85%) WITHIN 100 PC WITH LITTLE CONTAMINATION FROM DISTANT GIANTS. WE SUPPLEMENT WITH PS1 PHOTOMETRY TO IDENTIFY ADDITIONAL TARGETS WITH SMALLER PROPER-MOTIONS SELECTING ALL TARGETS WITH PS1 COLORS CONSISTENT WITH M DWARFS (FOLLOWING ALLER ET AL. 2013). WE PRIORITIZE OUR TARGETS BY COMPARING A NOMINAL EARTH-SIZED TRANSIT DEPTH TO OUR DEMONSTRATED PHOTOMETRIC PRECISION WITH K2 (R _EARTH COMES FROM TABULATED RELATIONS; BOYAJIAN ET AL. 2012). WE REQUIRE S/N&8 WITH KP<16 TO ALLOW FEASIBLE SPECTROSCOPIC FOLLOWUP. WE MINIMIZE BLENDS AND CONTAMINATION IN FIELD 7 (WHICH IS ESPECIALLY CROWDED) BY REJECTING ALL TARGETS WITH ANY 2MASS OR PS1 NEIGHBORS WITHIN 5 (THE RADIUS BEYOND WHICH OUR DATA VALIDATION CHECKS BECOME MOST EFFECTIVE). THESE SURVEYS HAVE A RESOLUTION OF 1 2 SO WE HAVE REMOVED ~90% OF CHANCE CLOSE ALIGNMENTS. THE FINAL RESULT IS 3733 M DWARF IN FIELDS 6&7 AROUND WHICH SMALL TRANSITS COULD BE IDENTIFIED WITH HIGH FIDELITY; MOST TARGETS ARE IN THE LESS-CROWDED FIELD 6. FIG. 2 SHOWS OUR SAMPLE S DEMOGRAPHICS. 2) DETECTION OF NEW EXOPLANETS - OUR DETECTION OF EXCITING PLANETARY SYSTEMS LIKE K2-3BCD (FIG. 1) DEMONSTRATES OUR TEAM S ABILITY TO RAPIDLY FIND AND CHARACTERIZE PLANETS TRANSITING K2 S M DWARFS. WE EXTRACT PHOTOMETRY FROM THE PIXEL DATA BUILDING ON THE WORK OF VANDERBURG&JOHNSON (2014) BUT WITH OPTIMIZATION OF APERTURE SIZE VS. FINAL RESIDUAL SCATTER. WE USE A GAUSSIAN PROCESS DECORRELATION APPROACH IN AN ITERATIVE FRAMEWORK WHICH IS HIGHLY INSENSITIVE TO STELLAR VARIABILITY ON THE&1 D TIMESCALES TYPICAL FOR M DWARFS. ANY STELLAR FLARES ARE APERIODIC AND ARE EASILY IDENTIFIED AS RAPID FLUX INCREASES INCONSISTENT WITH TRANSITS. WE WILL PROVIDE CALIBRATED LIGHT CURVES TO NEXSCI (SEE SEC. 6) SO OUR PROPOSAL OFFERS AN INDEPENDENT CHECK ON CALIBRATED LIGHT CURVES PROVIDES BY THE K2 MISSION. WE USE THE TERRA TRANSIT DETECTION PIPELINE (PETIGURA&MARCY 2012; PETIGURA ET AL. 2013B A) TO IDENTIFY TRANSIT-LIKE EVENTS FOR FURTHER VETTING INCLUDING BOTH PLANETS AND LARGE NUMBERS OF ECLIPSING BINARIES FOR OUR ANCILLARY SCIENCE CASE. 3) PLANET VALIDATION AND CHARACTERIZATION - DETECTION OF THE TRANSIT SIGNALS IN THE K2 LIGHT CURVES IS ONLY A FIRST STEP. TRANSIT CANDIDATES REQUIRE FOLLOW-UP OBSERVATIONS TO EXCLUDE FALSE POSITIVE DETECTIONS AND TO CHARACTERIZE THE REAL PLANETARY SYSTEMS. OUR FOLLOW-UP TEAM HAS EXTENSIVE EXPERIENCE OBSERVING CHARACTERIZING AND VALIDATING KEPLER CANDIDATES. WE ARE ALREADY FOLLOWING UP ~30 M DWARF SYSTEMS IN FIELD 1 A RATE COMPARABLE TO WHAT WE EXPECT IN FIELDS 6&7 (FIG. 2). OPTICAL AND INFRARED SPECTROSCOPY EFFICIENTLY CHARACTERIZES M DWARFS AND PROVIDES M _EARTH R _EARTH AND T EF F TO . 10% PRECISION. THE O/IR WAVELENGTHS PROVIDES NUMEROUS ATOMIC AND MOLECULAR FEATURES FOR BOLOMETRIC ANALYSES [FE/H] ACTIVITY AGE MASS AND RADII (MANN ET AL. 2013B; LEPINE ET AL. 2013; SCHLIEDER ET AL. 2012A). WE HAVE BEEN AWARDED A 70- NIGHT ESO LARGE PROGRAM (194.C-0443 PI CROSSFIELD) FOR 0.6 2.5 M MEDIUM-RESOLUTION SPECTROSCOPY OF ALL K2-MDP CANDIDATE HOSTS; WE HAVE ALREADY OBTAINED OIR PARAMETERS FOR ~50 M AND LATE K DWARFS IN BOTH PLANETARY AND EB SYSTEMS; THE ESO PROGRAM WILL CONTINUE THROUGH FIELDS 6&7 AND BEYOND. WE HAVE USED IRTF/SPEX (COLLABORATOR J. SCHLIEDER) AS DESCRIBED IN CROSSFIELD ET AL. (2015) AND ARE REQUESTING MORE IRTF TIME. GAIA DISTANCES WILL EVENTUALLY COMPLEMENT OUR SPECTRA WITH PRECISE HOST LUMINOSITIES; TOGETHER WITH OUR SPECTROSCOPY WE