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We disentangle X-ray disk reflection from complex line-of-sight absorption inthe nearby Seyfert NGC 4151, using a suite of Suzaku, NuSTAR, and XMM-Newtonobservations. Extending upon earlier published work, we pursue a physicallymotivated model using the latest angle-resolved version of the lamp-postgeometry reflection model relxillCp_lp together with a Comptonizationcontinuum. We use the long-look simultaneous Suzaku/NuSTAR observation todevelop a baseline model wherein we model reflected emission as a combinationof lamp-post components at the heights of 1.2 and 15.0 gravitational radii. Weargue for a vertically extended corona as opposed to two compact and distinctprimary sources. We find two neutral absorbers (one full-covering and onepartial-covering), an ionized absorber ($\log \xi = 2.8$), and a highly-ionizedultra-fast outflow, which have all been reported previously. All analyzedspectra are well described by this baseline model. The bulk of the spectralvariability between 1 keV and 6 keV can be accounted for by changes in thecolumn density of both neutral absorbers, which appear to be degenerate andinversely correlated with the variable hard continuum component flux. We trackvariability in absorption on both short (2 d) and long ($\sim$1 yr) timescales;the observed evolution is either consistent with changes in the absorberstructure (clumpy absorber at distances ranging from the broad line region(BLR) to the inner torus or a dusty radiatively driven wind) or a geometricallystable neutral absorber that becomes increasingly ionized at a rising fluxlevel. The soft X-rays below 1 keV are dominated by photoionized emission fromextended gas that may act as a warm mirror for the nuclear radiation.

A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151