We analyze Suzaku and XMM-Newton data of the highly variable Seyfert 2, IRAS 18325-5926. The spectra of the source are well modeled as a primary component described as an absorbed power law and a secondary power law component which is consistent with being scattered emission from an on-axis extended highly ionized medium. We show that while the primary component varies on a wide range of timescales from $10^{ 4} - 10^{ 8}$ s, the scattered emission is variable only on timescales longer than $10^{ 5}$ s. This implies that the extent of the scattering medium is greater than $10^{ 16}$ cm. The ratio of the scattered to primary flux ($\sim 0.03$) implies a column density for the scattering medium to be $\sim 10^{ 23}$ cm$^{ -2}$. We argue that for such a medium to be highly ionized it must be located less than $10^{ 17}$ cm from the X-ray source. Thus we localize the position and extent of scattering region to be $\sim$ a few $\times 10^{ 16}$ cm, with an average particle density of $\sim 10^{ 6}$ cm$^{ -3}$. We consider the physical interpretation of these results and as an aside, we confirm the presence of a broad Iron line emission in both the { \it XMM-Newton} and { \it Suzaku} observations.
Categories: astro-ph.CO astro-ph.HE