Virginia TechPonti, G.Cappi, M.Costantini, E.Bianchi, S.Kaastra, J. S.De Marco, B.Fender, R. P.Petrucci, P. O.Kriss, G. A.Steenbrugge, K. C.Arav, NahumBehar, E.Branduardi-Raymont, G.Dadina, M.Ebrero, J.Lubinski, P.Mehdipour, M.Paltani, S.Pinto, C.Tombesi, F.2013-12-062013-12-062013-01Ponti, G. ; Cappi, M. ; Costantini, E. ; et al., Jan. 2013. “Multiwavelength campaign on Mrk 509 XI. Reverberation of the Fe K alpha line,” ASTRONOMY & ASTROPHYSICS 549:A72. DOI: 10.1051/0004-6361/2012194500004-6361http://hdl.handle.net/10919/24439Context. We report on a detailed study of the Fe K emission/absorption complex in the nearby, bright Seyfert 1 galaxy Mrk 509. The study is part of an extensive XMM-Newton monitoring consisting of 10 pointings (~60 ks each) about once every 4 days, and includes a reanalysis of previous XMM-Newton and Chandra observations. Aims. We aim at understanding the origin and location of the Fe K emission and absorption regions. Results. Mrk 509 shows a clear (EW = 58 ± 4 eV) neutral Fe Kα emission line that can be decomposed into a narrow (σ = 0.027 keV) component (found in the Chandra HETG data) plus a resolved (σ = 0.22 keV) component. We find the first successful measurement of a linear correlation between the intensity of the resolved line component and the 3–10 keV flux variations on time scales of years down to a few days. The Fe Kα reverberates the hard X-ray continuum without any measurable lag, suggesting that the region producing the resolved Fe Kα component is located within a few light days to a week (r ≲ 103rg) from the black hole (BH). The lack of a redshifted wing in the line poses a lower limit of  ≥40 rg for its distance from the BH. The Fe Kα could thus be emitted from the inner regions of the BLR, i.e. within the  ~80 light days indicated by the Hβ line measurements. In addition to these two neutral Fe Kα components, we confirm the detection of weak (EW ~ 8–20 eV) ionised Fe K emission. This ionised line can be modelled with either a blend of two narrow Fe xxv and Fe xxvi emission lines (possibly produced by scattering from distant material) or with a single relativistic line produced, in an ionised disc, down to a few rg from the BH. In the latter interpretation, the presence of an ionised standard α-disc, down to a few rg, is consistent with the source high Eddington ratio. Finally, we observe a weakening/disappearing of the medium- and high-velocity high-ionisation Fe K wind features found in previous XMM-Newton observations. Conclusions. This campaign has made the first reverberation measurement of the resolved component of the Fe Kα line possible, from which we can infer a location for the bulk of its emission at a distance of r ~ 40–1000 rg from the BH.en-USIn Copyrightaccretionaccretion disksblack hole physicsmethods: data analysisgalaxies: individual: Mrk 509galaxies: active: galaxies: Seyfertactive galactic nucleix-ray reverberationblack-hole massseyfert 1galaxiesbroad iron linesxmm-newtonabsorption-lineswarm absorbersemission-lineaccretion disksAstronomy & AstrophysicsArticle - Refereedhttp://www.aanda.org/articles/aa/abs/2013/01/aa19450-12/aa19450-12.htmlhttps://doi.org/10.1051/0004-6361/201219450