DIELECTRONIC RECOMBINATION OF Fe 3p IONS: A KEY INGREDIENT FOR DESCRIBING X-RAY ABSORPTION IN ACTIVE GALACTIC NUCLEI

We have carried-out multi-configuration Breit–Pauli autostructure calculations for the dielectronic recombination (DR) of Fe – Fe ions. We obtain total DR rate coefficients for the initial ground-level which are an order of magnitude larger than those corresponding to radiative recombination (RR), at temperatures where Fe 3p (q = 2 − 6) ions are abundant in photoionized plasmas. The resultant total (DR+RR) rate coefficients are then an order of magnitude larger than those currently in use by photoionized plasma modeling codes such as cloudy, ion and xstar. These rate coefficients, together with our previous results for q = 0 and 1, are critical for determining the ionization balance of the M-shell Fe ions which give rise to the prominent unresolved-transition-array X-ray absorption feature found in the spectrum of many active galactic nuclei. This feature is poorly described by cloudy and ion, necessitating an ad hoc modification to the low-temperature DR rate coefficients. Such modifications are no longer necessary and a rigorous approach to such modeling can now take place using these data. Subject headings: atomic data – atomic processes – galaxies: active – galaxies: nuclei – X-rays: galaxies