NARROW-LINE SEYFERT LS ARE A LINCHPIN TO OUR UNDERSTANDING OF THE PHYSICS OF ACCRETION IN SUPERMASSIVE BLACK HOLES AS THEY PROVIDE A DIRECT VIEW OF THE INNERMOST REGIONS AT THE INTERSECTION OF GAS INFALL AND OUTFLOW. THIS IS ESPECIALLY TRUE FOR THE NEWLY DISCOVERED SUBCLASS OF GAMMA-RAY LOUD NLSLS WHICH IN ADDITION TO THEIR NEAR-EDDINGTON LUMINOSITIES ALSO SHOW CLEAR EVIDENCE FOR MECHANICAL OUTFLOWS IN THE FORM OF RELATIVISTIC JETS. IT IS DEBATED WHETHER THE X-RAY EMISSION IN THESE OBJECTS ORIGINATES IN THE DISC/CORONA OR IF IT IS PRODUCED FURTHER OUT IN THE JET. WE PROPOSE TO BREAK THIS DEGENERACY BY SEARCHING FOR X-RAY REVERBERATION LAGS AND ULTRAFAST OUTFLOWS IN THE PROTOTYPE GAMMA-RAY LOUD NLSL 1H0323+342. IF SHORT TIMESCALE LAGS EXIST BETWEEN THE CONTINUUM AND SOFT EXCESS AND/OR IRON K LINE THIS WILL SUGGEST THAT THE ORIGIN OF THE X-RAY EMISSION IS THE CORONA LEADING TO A BETTER UNDERSTANDING OF THE DISC CORONA WIND JET CONNECTION IN SUPERMASSIVE BLACK HOLES. WE REQUEST 250 KS OF XMM-NEWTON AND 125 KS OF NUSTAR TIME. 2. DESCRIPTION OF THE PROPOSED PROGRAMME A) SCIENTIFIC RATIONALE: NARROW-LINE SEYFERT 1 GALAXIES (NLSLS) WERE INITIALLY CLASSIFIED FOR THEIR STRIKING OPTICAL PROPERTIES-NARROW HP LINES WEAK [OIII] AND STRONG FELL LINES (OSTERBROCK&POGGE 1985) WHICH SUGGESTED THESE ACTIVE GALACTIC NUCLEI CONTAINED RELATIVELY SMALL SUPERMASSIVE BLACK HOLES ACCRETING NEAR OR ABOVE THE EDDINGTON LIMIT (BOROSON&GREEN 1992). BECAUSE OF THIS THEY ARE THOUGHT TO BE AT AN EARLY PHASE IN THEIR AGN EVOLUTION BEFORE DEVELOPING INTO MORE MASSIVE LUMINOUS QUASARS. IN ADDITION TO THEIR UNIQUE OPTICAL SPECTRA NLSLS SHOW INTERESTING X-RAY BEHAVIOR INCLUDING RAPID VARIABILITY A SOFT EXCESS AND OFTEN STRONG REFLECTION FEATURES SUGGESTING THAT WE HAVE A LINE-OF-SIGHT DIRECTLY TOWARDS THE INNER ACCRETION FLOW AND CORONA. BECAUSE OF THEIR LOW MASS BLACK HOLES THE VARIABILITY TIMESCALES IN NLSLS ARE SHORT ENOUGH TO PROBE IN A SINGLE OBSERVATION WITH.XMM-NEWTON. IN RECENT YEARS FOURIER-BASED TIMING ANALYSES OF RAPIDLY VARIABLE NLSLS HAVE REVEALED X-RAY REVERBERATION LAGS WHERE THE REFLECTION FEATURES (I.E. THE IRON K EMISSION LINE AND COMPTON HUMP) ARE DELAYED WITH RESPECT TO THE X-RAY CONTINUUM DUE TO THE ADDITIONAL LIGHT TRAVEL PATH OF THE REFLECTED PHOTONS (UTTLEY ET AL. 2014 FOR REVIEW). THE SHORT TIMESCALE OF THE LAGS INDICATES THAT THE CENTRAL CORONA IS GEOMETRICALLY COMPACT AND THAT THE REPROCESSING REGION IS CLOSE TO THE CENTRAL BLACK HOLE WITHIN .. 10 GRAVITATIONAL RADII (SEE EXAMPLE IN FIG. 1 KARA ET AL. 2013). MOST NLSLS SHOW NO EVIDENCE FOR JETS HOWEVER RECENTLY THE PENNI-GAMMA-RAY SPACE TELESCOPE HAS DISCOVERED A NEW SUBCLASS OF NLSLS: GAMMA-RAY-LOUD NLSLS WHICH SHOW HYBRID CHARACTERISTICS BOTH OF NLSLS ( E.G. LOW MASS BLACK HOLE HIGH ACCRETION RATE SPIRAL GALAXY HOST) AND BLAZARS E.G. FLAT RADIO SPECTRA HIGH BRIGHTNESS TEMPERATURES (ZHOU ET AL. 2003) AND IN SOME CASES SUPERLUMINAL MOTION SEEN IN RADIO IMAGES (D'AMMANDO ET AL. 2012). HIGHLY ACCRETI~G NLSLS ARE NOT THE CLASSICAL ENVIRONMENTS FOR RELATIVISTIC JETS TO DEVELOP AND SO STUDYING THIS NEW CLASS OF OBJECTS CAN GIVE US CLUES INTO THE FORMATION AND EVOLUTION OF EXTRAGALACTIC JETS ESPECIALLY IF NLSLS REPRESENT A YOUNG AGN POPULATION. THE PROTOTYPE GAMMA-RAY LOUD NLSL IS 1H0323+342 (Z 0.06 ZHOU ET AL. 2007). IN ADDITION TO ITS VARIABLE GAMMA-RAY EMISSION IT ALSO SHOWS CLEAR SIGNS OF SUPERLUMINAL MOTION {1-7C) IN ITS RADIO IMAGES SUGGESTING A RELATIVISTIC JET AT A VIEWING ANGLE OF (J 4 - 13 DEG {FIG. 2-CENTER FUHRMANN ET AL 2015). ITS DOUBLE-PEAKED SED {IN RADIO-INFRARED AND IN GEV GAMMA-RAYS) CAN BE EXPLAINED WITH NON-THERMAL JET EMISSION (FIG 2-LEFT).