Is XRISM/Resolve probing a "raining" absorber in Mrk 509?

Abstract

X-ray spectroscopy of AGN offers unique insights into the reprocessing of radiationand gas dynamics near SMBH. The Sey 1 galaxy Mrk 509 is an ideal laboratory for these studies since its complex FeK$\hat{I}\pm$ in emission and the past evidences of transient and fast flows. We present the first high-resolution 2-12 keV spectrum of Mrk 509 obtained with the Resolve calorimeter on-board XRISM, complemented with XMM-Newton and NuSTAR observations to constrain the broadband continuum. We modeled the spectra using self-consistent reflection models for the continuum and emission lines, and photoionized plasma models for the absorption components. The XRISM/Resolve spectrum reveals a narrow FeK$\hat{I}\pm$ core resolved with $\ddot{I}ƒ\sim 10eV$ (v${}_{FWHM}\sim$ 1100 km/s) and a broader component with $\ddot{I}ƒ\sim 450eV$. We also find tentative evidence (3.6$\ddot{I}ƒ$) for a ionized absorber. The data suggest that this component is infalling with a velocity of $v_{in}\sim 11000$ km/s and that it is located within few thousands gravitational radii. The narrow FeK$\hat{I}\pm$ emission is consistent with an origin in the dusty torus, while the broad component arises from the inner BLR or in the accretion disk (R$\sim 30--120r_g$). Relativistic reflection modeling indictaes the inner edge if the emitting disk to R$\ge 27r_g$. If confirmed, the high velocity inflow would likely represent fragmented clumps of a "failed wind" raining onto the accretion disk. providing potential direct evidence that non-standard accretion processes coexist with canonical disk-like flows in the inner regions of AGNS.

Accepted for publication on A&A