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Complex narrow line Seyfert 1s (NLS1s), such as 1H0707-495, differ fromsimple NLS1s like PG1244+026 by showing stronger broad spectral features at FeK and larger amplitude flux variability. These are correlated: the strongest FeK features are seen during deep dips in the light curves of complex NLS1s.There are two competing explanations for these features, one where a compactX-ray source on the spin axis of a highly spinning black hole approaches thehorizon and the consequent strong relativistic effects focus the intrinsic fluxonto the inner edge of a thin disc, giving a dim, reflection dominatedspectrum. The other is that the deep dips are caused by complex absorption byclumps close to the hard X-ray source. The reflection dominated model is ableto reproduce the very short 30s soft lag from reverberation seen in the complexNLS1 1H0707-495. However, it does not explain the characteristic switch to hardlags on longer timescales. Instead, a full model of propagating fluctuationscoupled to reverberation can explain the switch in the simple NLS1 PG1244+026using a low spin black hole. However PG1244+026 has a longer reverberation lagof $\sim 200$s.  Here we extend the successful propagation-reverberation model for the simpleNLS1 PG1244+026 to include the effect of absorption from clumps in a turbulentregion above the disk. The resulting occultations of the inner accretion flowcan introduce additional hard lags when relativistic effects are taken intoaccount. This dilutes the soft lag from reverberation and shifts it to higherfrequencies, making a smooth transition between the 200s lags seen in simpleNLS1s to the 30s lags in complex NLS1s. These two classes of NLS1 could then bedetermined by inclination angle with respect to a clumpy, probably turbulent,failed wind structure on the disc.

Complex Narrow Line Seyfert 1s: High spin or high inclination?