Localizing narrow Fe Kαemission within bright AGN

Context.The 6.4 keV Fe Kαemission line is a ubiquitous feature in X-ray spectra of active galactic nuclei (AGN), and its properties track the interaction between the variable primary X-ray continuum and the surrounding structure from which it arises.Aims.We clarify the nature and origin of the narrow Fe Kαemission using X-ray spectral, timing, and imaging constraints, plus possible correlations to AGN and host galaxy properties, for 38 bright nearby AGN (z Methods.ModelingChandraandXMM-Newtonspectra, we computed line full-width half-maxima (FWHMs) and constructed Fe Kαline and 2–10 keV continuum light curves. The FWHM provides one estimate of the Fe Kαemitting region size,RFeKα, assuming virial motion. A second estimate comes from comparing the degree of correlation between the variability of the continuum and line-only light curves, compared to simulated light curves. Finally, we extractedChandraradial profiles to place upper limits onRFeKα.Results.For 90% (21/24) of AGN with FWHM measurements,RFeKαis smaller than the fiducial dust sublimation radius,Rsub. From timing analysis, 37 and 18 AGN show significant continuum and Fe Kαvariability, respectively. Despite a wide range of variability properties, the constraints on the Fe Kαphoton reprocessor size independently confirm thatRFeKαis smaller thanRsubin 83% of AGN. Finally, the imaging analysis yields loose upper limits for all but two sources; notably, the Circinus Galaxy and NGC 1068 show significant but subdominant extended Fe Kαemission out to ∼100 and ∼800 pc, respectively.Conclusions.Based on independent constraints, we conclude that the majority of the narrow Fe Kαemission in typical AGN predominantly arises from regions smaller than and presumably insideRsub, and thus it is associated either with the outer broad line region or outer accretion disk. However, the large diversity of continuum and narrow Fe Kαvariability properties are not easily accommodated by a universal scenario.