XRISM/Resolve probes a possible “raining” absorber in Mrk 509
Abstract
Context. X-ray spectroscopy of active galactic nuclei (AGNs) offers unique insights into the reprocessing of radiation and the gas dynamics near supermassive black holes. The Seyfert 1 galaxy Mrk 509 is an ideal laboratory for these studies. It is in fact known for its complex iron K emission and one of the four or five AGNs to date in which evidence of transient, blue- and redshifted absorption features indicative of high-velocity flows has been detected in X-rays. Aims. We present the first high-resolution 2–10 keV spectrum of Mrk 509 obtained with the XRISM /Resolve calorimeter. Our primary goals are to disentangle the narrow and broad emission features and to place stringent constraints on the kinematics and physical locations of circumnuclear gas flows, specifically searching for signatures of accretion and feedback. Methods. We analyzed 106 ks of XRISM/Resolve data, complemented by simultaneous XMM-Newton and NuSTAR observations, which we used to constrain the broadband continuum. We modeled the spectra using self-consistent reflection models for the continuum and the emission lines, and employed photoionized plasma models to characterize discrete, ionized absorption features. Results. The XRISM/Resolve spectrum reveals a narrow Fe K α core resolved with σ ≃ 10 eV ( v FWHM ∼ 1100 km/s). The best-fit model includes a broader component with σ ∼ 450 eV. We also find tentative evidence of discrete absorption features at rest-frame energies of E ∼ 6.2 keV. When modeled as an ionized absorber (with a significance of ∼3.6 σ ), the data suggest the gas is redshifted relative to the systemic velocity, corresponding to an inflow of material with v in ∼ 11 000 km s −1 , located within the inner few thousand gravitational radii. Conclusions. The narrow Fe K α emission is consistent with an origin in the dusty torus, while the broad component arises from broad-line-region scales or the accretion disk ( R ∼ 30–120 r g ). This scenario is strongly corroborated by our relativistic reflection modeling, which restricts the inner edge of the emitting region to distances greater than 27 r g . If confirmed by future observations, the high-velocity inflow would likely represent dense, fragmented clumps of a “failed wind” raining back onto the accretion disk, providing potential direct evidence that nonstandard accretion processes may coexist with canonical disk-like flows in the inner regions of AGNs.
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BibTeX
@article{dadina2026xrismresolve,
title = {{XRISM/Resolve probes a possible “raining” absorber in Mrk 509}},
author = {M. Dadina and V. Missaglia and V. Braito and M. Cappi and A. Luminari and Didier Barret and E. Bertola and S. Bianchi and A. Comastri and G. Chartas and J. Kaastra and E. Kammoun and G. Lanzuisi and G. Matzeu and R. Middei and E. Nardini and F. Nicastro and P.-O. Petrucci and C. Pinto and R. Serafinelli and A. Tortosa and C. Vignali},
journal = {Astronomy \& Astrophysics - A\&A},
year = {2026},
month = jul,
doi = {10.1051/0004-6361/202659563},
url = {https://hal.science/hal-05847344v1},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - XRISM/Resolve probes a possible “raining” absorber in Mrk 509
AU - M. Dadina
AU - V. Missaglia
AU - V. Braito
AU - M. Cappi
AU - A. Luminari
AU - Didier Barret
AU - E. Bertola
AU - S. Bianchi
AU - A. Comastri
AU - G. Chartas
AU - J. Kaastra
AU - E. Kammoun
AU - G. Lanzuisi
AU - G. Matzeu
AU - R. Middei
AU - E. Nardini
AU - F. Nicastro
AU - P.-O. Petrucci
AU - C. Pinto
AU - R. Serafinelli
AU - A. Tortosa
AU - C. Vignali
PY - 2026
DA - 2026/07/01
JO - Astronomy & Astrophysics - A&A
DO - 10.1051/0004-6361/202659563
UR - https://hal.science/hal-05847344v1
AB - Context. X-ray spectroscopy of active galactic nuclei (AGNs) offers unique insights into the reprocessing of radiation and the gas dynamics near supermassive black holes. The Seyfert 1 galaxy Mrk 509 is an ideal laboratory for these studies. It is in fact known for its complex iron K emission and one of the four or five AGNs to date in which evidence of transient, blue- and redshifted absorption features indicative of high-velocity flows has been detected in X-rays. Aims. We present the first high-resolution 2–10 keV spectrum of Mrk 509 obtained with the XRISM /Resolve calorimeter. Our primary goals are to disentangle the narrow and broad emission features and to place stringent constraints on the kinematics and physical locations of circumnuclear gas flows, specifically searching for signatures of accretion and feedback. Methods. We analyzed 106 ks of XRISM/Resolve data, complemented by simultaneous XMM-Newton and NuSTAR observations, which we used to constrain the broadband continuum. We modeled the spectra using self-consistent reflection models for the continuum and the emission lines, and employed photoionized plasma models to characterize discrete, ionized absorption features. Results. The XRISM/Resolve spectrum reveals a narrow Fe K α core resolved with σ ≃ 10 eV ( v FWHM ∼ 1100 km/s). The best-fit model includes a broader component with σ ∼ 450 eV. We also find tentative evidence of discrete absorption features at rest-frame energies of E ∼ 6.2 keV. When modeled as an ionized absorber (with a significance of ∼3.6 σ ), the data suggest the gas is redshifted relative to the systemic velocity, corresponding to an inflow of material with v in ∼ 11 000 km s −1 , located within the inner few thousand gravitational radii. Conclusions. The narrow Fe K α emission is consistent with an origin in the dusty torus, while the broad component arises from broad-line-region scales or the accretion disk ( R ∼ 30–120 r g ). This scenario is strongly corroborated by our relativistic reflection modeling, which restricts the inner edge of the emitting region to distances greater than 27 r g . If confirmed by future observations, the high-velocity inflow would likely represent dense, fragmented clumps of a “failed wind” raining back onto the accretion disk, providing potential direct evidence that nonstandard accretion processes may coexist with canonical disk-like flows in the inner regions of AGNs.
SN - 0004-6361
SN - 1432-0746
ER -