Another X-ray UFO without a momentum-boosted molecular outflow

Bonanomi, F.; Cicone, C.; Severgnini, P.; Braito, V.; Vignali, C.; Reeves, J. N.; Sirressi, Mattia; Arroyave, I. Montoya; Ceca, R. Della; Ballo, L.; Dotti, Massimo

doi:10.1051/0004-6361/202245630

Cited by 5 publications

(1 citation statement)

References 81 publications

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“…UFOs probe nuclear flows, and they therefore most likely belong to the momentum-driven regime. It is thus expected that most of the sources in compilations of UFOs and galaxy-scale outflows are compatible with momentum-driven flows (e.g., Bonanomi et al 2023). Because nuclear wind is likely short lived, the observed UFOs may well not be causally related with the more long-lived galaxy-scale winds.…”

Section: Radiation-driven Disk-wind Scenariomentioning

confidence: 99%

Dynamical complexity in microscale disk-wind systems

Fiore,

Gaspari,

Luminari

et al. 2024

A&A

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Powerful winds at accretion-disk scales have been observed in the past 20 years in many active galactic nuclei (AGN). These are the so-called ultrafast outflows (UFOs). Outflows are intimately related to mass accretion through the conservation of angular momentum, and they are therefore a key ingredient of most accretion disk models around black holes (BHs). At the same time, nuclear winds and outflows can provide the feedback that regulates the joint BH and galaxy growth. We reconsidered UFO observations in the framework of disk-wind scenarios, both magnetohydrodynamic disk winds and radiatively driven winds. We studied the statistical properties of observed UFOs from the literature and derived the distribution functions of the ratio $ of the mass-outflow and -inflow rates and the ratio $ of the mass-outflow and the Eddington accretion rates. We studied the links between $ and $ and the Eddington ratio $ L_ bol L_ Edd $. We derived the typical wind-activity history in our sources by assuming that it can be statistically described by population functions. We find that the distribution functions of $ and $ can be described as power laws above some thresholds, suggesting that there may be many wind subevents for each major wind event in each AGN activity cycle, which is a fractal behavior. We then introduced a simple cellular automaton to investigate how the dynamical properties of an idealized disk-wind system change following the introduction of simple feedback rules. We find that without feedback, the system is overcritical. Conversely, when feedback is present, regardless of whether it is magnetic or radiation driven, the system can be driven toward a self-organized critical state. Our results corroborate the hypothesis that AGN feedback is a necessary key ingredient in disk-wind systems, and following this, in shaping the coevolution of galaxies and supermassive BHs.

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Section: Radiation-driven Disk-wind Scenariomentioning

confidence: 99%

Dynamical complexity in microscale disk-wind systems

Fiore,

Gaspari,

Luminari

et al. 2024

A&A

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Winds of change: The nuclear and galaxy-scale outflows and the X-ray variability of 2MASS 0918+2117

Baldini,

Lanzuisi,

Brusa

et al. 2024

A&A

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In this work, we test feedback propagation models on the test case of 2MASS 0918+2117 (2M0918), a z=0.149 X-ray variable AGN that shows tentative evidence for nuclear ultra-fast outflows (UFOs) in a 2005 XMM-Newton observation. We also investigate whether UFOs can be related to the observed X-ray variability. We observed 2M0918 with XMM-Newton and NuSTAR in 2020 to confirm the presence of and characterize the UFOs. We performed a kinematic analysis of the publicly available 2005 SDSS optical spectrum to reveal and measure the properties of galaxy-scale ionized outflows. black Furthermore, we constructed 20-year-long light curves of observed flux, line-of-sight column density, and intrinsic accretion rate from the spectra of the first four SRG /eROSITA all-sky surveys and archival observations from Chandra and XMM-Newton We detect UFOs with vsim 0.16c and galaxy-scale ionized outflows with velocities of sim 700 km/s. We also find that the drastic X-ray variability (factors >10) can be explained in terms of variable obscuration and variable intrinsic luminosity. black Comparing the energetics of the two outflow phases, 2M0918 is consistent with momentum-driven wind propagation. 2M0918 expands the sample of AGN with both UFOs and ionized gas winds from 5 to 6 and brings the sample of AGN hosting multiscale outflows to 19, contributing to a clearer picture of feedback physics. From the variations in accretion rate, column density, and ionization level of the obscuring medium, we propose a scenario that connects obscurers, an accretion enhancement, and the emergence of UFOs.

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The XMM-Newton and NuSTAR view of IRASF11119+3257

Lanzuisi,

Matzeu,

Baldini

et al. 2024

A&A

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IRASF11119+3257 is an ultra-luminous infrared galaxy with a post-merger morphology, hosting a type-1 quasar at z=0.189. It shows a prominent ultra-fast outflow (UFO) absorption feature ($ in its 2013 spectrum. This is the first system in which the energy released by the UFO was compared to that of the known galaxy-scale molecular outflow to investigate the mechanism driving active galactic nuclei (AGN) feedback. In 2021, we obtained the first long look of the target, coordinated with a simultaneous observation, with the goal of constraining the broad band continuum and the nuclear wind physical properties and energetics with an unprecedented accuracy. The new high-quality data allowed us to clearly detect at a confidence level $P>99.8<!PCT!>$ multiple absorption features associated with the known UFO at the 9.1 and 11.0 keV rest frames. Furthermore, an emission plus absorption feature at $1.1-1.3$ keV reveals the presence of a blueshifted P-Cygni profile in the soft band. We associate the two hard band features with blends of FeXXV and FeXXVI and line pairs and infer a large column ($ $ cmsq ) of highly ionized ($log gas outflowing at $ The 1.3 keV absorption line can be associated with a blend of Fe and Ne transitions, produced by a lower column ($ $ cmsq ) and ionization ($log gas component outflowing at the same speed. Using a radiative-transfer disk wind model to fit the highly ionized UFO, we derive a mass outflow rate comparable with the mass accretion rate and the Eddington limit ($ macc and $ medd ), and kinetic energy ($ and $ and momentum flux ($ among the highest reported in the literature. We measured an extremely low high-energy cutoff ($ keV). This and several other cases in the literature suggest that a steep X-ray continuum may be related to the formation of powerful winds. We also analyzed the ionized OIII component of the large-scale outflow through optical spectroscopy and derived a large outflow velocity ($ km/s) and energetics comparable with the large-scale molecular outflows. Finally, we observe a trend of decreasing outflow velocity from forbidden optical emission lines of decreasing ionization levels, interpreted as the outflow decelerating at large distances from the ionizing source. The lack of a significant momentum boost between the nuclear UFO and the different phases of the large-scale outflow, observed in IRASF11119 and in a growing number of similar sources, can be explained by (i) a momentum-driven expansion, (ii) an inefficient coupling of the UFO with the host interstellar medium, or (iii) by repeated energy-driven expansion episodes with a low duty cycle, that average out on long timescales to produce the observed large-scale outflow.

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Another X-ray UFO without a momentum-boosted molecular outflow

Cited by 5 publications

References 81 publications

Dynamical complexity in microscale disk-wind systems

Dynamical complexity in microscale disk-wind systems

Winds of change: The nuclear and galaxy-scale outflows and the X-ray variability of 2MASS 0918+2117

The XMM-Newton and NuSTAR view of IRASF11119+3257

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