Supermassive Black Hole Winds in X-rays: SUBWAYS

Matzeu, G. A.; Brusa, M.; Lanzuisi, G.; Dadina, M.; Bianchi, S.; Kriss, G. A.; Mehdipour, M.; Nardini, E.; Chartas, G.; Middei, R.; Piconcelli, E.; Gianolli, Vittoria E.; Comastri, A.; Longinotti, A. L.; Krongold, Y.; Ricci, F.; Petrucci, Pierre-Olivier; Tombesi, Francesco; Luminari, A.; Zappacosta, L.; Miniutti, G.; Gaspari, M.; Behar, E.; Bischetti, M.; Mathur, S.; Perna, M.; Giustini, M.; Grandi, P.; Torresi, E.; Vignali, C.; Bruni, G.; Cappi, M.; Costantini, E.; Cresci, G.; Marco, Barbara De; Rosa, A. De; Gilli, R.; Guainazzi, M.; Kaastra, J. S.; Kraemer, Steve; Franca, F. La; Marconi, A.; Panessa, F.; Ponti, G.; Proga, Daniel; Ursini, F.; Baldini, Paolo; Fiore, F.; King, Andrew; Maiolino, R.; Matt, Giorgio; Merloni, A.

doi:10.1051/0004-6361/202245036

Cited by 23 publications

(3 citation statements)

References 181 publications

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“…They are now observed in different gas phases and on different physical scales, from parsec-scale ultrafast (∼10% of the speed of light) outflows detected in X-rays (e.g. Pounds et al 2003;Nardini et al 2015;Matzeu et al 2023) to kiloparsec-scale outflows observed in atomic, molecular, and ionised gas with velocities up to ∼1000 km s −1 (e.g. Rupke & Veilleux 2011;Cicone et al 2014;Carniani et al 2015;Harrison et al 2016;Förster Schreiber et al 2019;Kakkad et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Bubbles and outflows: The novel JWST/NIRSpec view of the z = 1.59 obscured quasar XID2028

Cresci

Tozzi

Perna

et al. 2023

A&A

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Quasar feedback in the form of powerful outflows is invoked as a key mechanism to quench star formation in galaxies, although direct observational evidence is still scarce and debated. Here we present Early Release Science JWST NIRSpec IFU observations of the z = 1.59 prototypical obscured Active Galactic Nucleus (AGN) XID2028: This target represents a unique test case for studying quasar feedback at the peak epoch of AGN-galaxy co-evolution because extensive multi-wavelength coverage is available and a massive and extended outflow is detected in the ionised and molecular components. With the unprecedented sensitivity and spatial resolution of the JWST, the NIRSpec dataset reveals a wealth of structures in the ionised gas kinematics and morphology that were previously hidden in the seeing-limited ground-based data. In particular, we find evidence of an interaction between the interstellar medium of the galaxy and the quasar-driven outflow and radio jet that produces an expanding bubble from which the fast and extended wind detected in previous observations emerges. The new observations confirm the complex interplay between the AGN jet, wind and the interstellar medium of the host galaxy, highlighting the role of low-luminosity radio jets in AGN feedback. They also clearly show the new window that NIRSpec opens for detailed studies of feedback at high redshift.

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Section: Introductionmentioning

confidence: 99%

Bubbles and outflows: The novel JWST/NIRSpec view of the z = 1.59 obscured quasar XID2028

Cresci

Tozzi

Perna

et al. 2023

A&A

Self Cite

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“…In the ω and λ w ranges 0.007-0.14 and 0.004-0.04, the differential distributions are flat, with a slope consistent with 0. The application in the next years of this type of analysis to less biased and complete AGN samples, such as the SUBWAYS sample (Mehdipour et al 2022;Matzeu et al 2023) is crucial to reduce the statistical and systematic uncertainties.…”

Section: Population Properties Versus Single-system Evolutionmentioning

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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“…The third one is the ultrafast outflow (UFO). Seyfert galaxies often have blueshifted, highly ionized iron K-absorption lines in their 30%-40% of the X-ray spectra (Tombesi et al 2010;Gofford et al 2013;Igo et al 2020;Matzeu et al 2023). UFOs are considered to be outflowing winds from the accretion disk at very high velocities of 0.1-0.3c, where c is the speed of light.…”

Section: Introductionmentioning

confidence: 99%

Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809

Midooka,

Mizumoto,

Ebisawa

2023

ApJ

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Recent radiation-magnetohydrodynamic simulations of active galactic nuclei predict the presence of the disk winds, which may become unstable and turn into fragmented clumps far from the central black hole. These inner winds and the outer clumps may be observed as ultrafast outflows (UFOs) and partial absorbers, respectively. However, it is challenging to observationally constrain their origins because of the complicated spectral features and variations. To resolve such degeneracies of the clumpy absorbers and other components, we developed a novel spectral-ratio model fitting technique that estimates the variable absorbing parameters from the ratios of the partially absorbed spectra to the non-absorbed one, canceling the complex non-variable spectral features. We applied this method to the narrow-line Seyfert 1 galaxy IRAS 13224-3809 observed by XMM-Newton in 2016 for ∼1.5 Ms. As a result, we found that the soft spectral variation is mostly caused by changes in the partial covering fraction of the mildly ionized clumpy absorbers, whose outflow velocities are similar to those of the UFO (∼0.2–0.3c). Furthermore, the velocities of the clumpy absorbers and UFOs increase similarly with the X-ray fluxes, consistent with the change in the UV-dominant continuum flux. We also discovered a striking correlation between the clump covering fraction and the equivalent width of the UFO absorption lines, which indicates that increasing the outflow in the line of sight leads to more prominent UFOs and more partial absorption. These findings strongly suggest that the clumpy absorbers and the UFO share the same origin, driven by the same UV-dominant continuum radiation.

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Supermassive Black Hole Winds in X-rays: SUBWAYS

Cited by 23 publications

References 181 publications

Bubbles and outflows: The novel JWST/NIRSpec view of the z = 1.59 obscured quasar XID2028

Bubbles and outflows: The novel JWST/NIRSpec view of the z = 1.59 obscured quasar XID2028

Dynamical complexity in microscale disk-wind systems

Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809

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