Kinetic Energy Transfer from X-Ray Ultrafast Outflows to Millimeter/Submillimeter Cold Molecular Outflows in Seyfert Galaxies

Mizumoto, Misaki; Izumi, Teruo; Kohno, Kotaro

doi:10.3847/1538-4357/aaf814

Cited by 32 publications

(49 citation statements)

References 42 publications

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“…This is consistent with the recent analysis of Mizumoto et al (2019), who analyzed a small Xray sample of 8 AGN (including I Zw 1), selected from the Cicone et al (2014) CO sample. Mizumoto et al (2019) inferred that the energy transfer rate, from the black hole wind to the molecular gas, spanned a wide range of efficiency from ǫ ∼ 7 × 10 −3 − 1 (where ǫ = 1 corresponds to a perfectly energy conserving outflow). Similarly, the AGN outflows compiled by Fiore et al (2017) show a wide range of momentum load factors, with about half of the AGN receiving a boost of at least ×10 in the molecular outflow component compared to the X-ray wind.…”

Section: Comparison With the Molecular Gas Outflowssupporting

confidence: 91%

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

Reeves

Braito

2019

ApJ

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I Zw 1 is the prototype optical narrow line Seyfert 1 galaxy. It is also a nearby (z = 0.0611), luminous QSO, accreting close to the Eddington limit. XMM-Newton observations of I Zw 1 in 2015 reveal the presence of a broad and blueshifted P-Cygni iron K profile, as observed through a blue-shifted absorption trough at 9 keV and a broad excess of emission at 7 keV in the X-ray spectra. The profile can be well fitted with a wide angle accretion disk wind, with an outflow velocity of at least −0.25c. In this respect, I Zw 1 may be an analogous to the prototype fast wind detected in the QSO, PDS 456, while its overall mass outflow rate is scaled down by a factor ×50 due to its lower black hole mass. The mechanical power of the fast wind in I Zw 1 is constrained to within 5 − 15% of Eddington, while its momentum rate is of the order unity. Upper-limits placed on the energetics of any molecular outflow, from its CO profile measured by IRAM, appear to rule out the presence of a powerful, large scale, energy conserving wind in this AGN. We consider whether I Zw 1 may be similar to a number of other AGN, such as PDS 456, where the large scale galactic outflow is much weaker than what is anticipated from models of energy conserving feedback.

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Section: Comparison With the Molecular Gas Outflowssupporting

confidence: 91%

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

Reeves

Braito

2019

ApJ

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“…Remarkably, this is at tension with a classic energy-conserving 4 In NGC 6240 the α ou t C O estimated for the outflow is lower than the α C O estimated for the non-outflowing H 2 gas reservoir, as expected if the large σ v of the clouds in outflow partially decrease the optical depth of its global low-J CO emission (Cicone et al 2018) (1) Outflow type; (2) blast-wave feedback scenario which predicts not only the kinetic power to be conserved but also the momentum rate of the large scale outflow to be boosted (Faucher-Giguère & Quataert 2012). The efficiency factor, which we define as the ratio between the kinetic power of the molecular outflow to the X-ray wind, is E mol / E U FO ∼ 4 · 10 −3 , lower than the range found by Mizumoto et al (2019) for a sample of six Seyfert galaxies, i.e. from ∼ 7 · 10 −3 to ∼ 1.…”

Section: Testing the Agn Feedback Scenariomentioning

confidence: 67%

“…Furthermore, in IRAS F11119+3257, new ALMA data allowed to revise the estimate of the momentum rate of the molecular outflow, finding that this source may be more consistent with the momentum-conserving feedback scenario, contrary to previous claims (see Veilleux et al 2017). Finally, Mizumoto et al (2019) measured a wide range of values for the ratios between the kinetic powers of molecular outflows to the X-ray UFOs, studying a sample of six ULIRGs and quasar-hosts where both an X-ray wind and a molecular outflow have been detected. These findings, together with our new results, point out that the relation (if any) between the disk-wind and the large-scale ISM is more complex than commonly assumed.…”

Section: Testing the Agn Feedback Scenariomentioning

confidence: 99%

Testing the blast-wave AGN feedback scenario in MCG-03-58-007

Sirressi

Cicone

Severgnini

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report the first Atacama large millimeter/submillimeter array observations of MCG-03-58-007, a local (z = 0.03236±0.00002, this work) AGN (L AG N ∼ 10 45 erg s −1 ), hosting a powerful X-ray ultra-fast (v = 0.1c) outflow (UFO). The CO(1-0) line emission is observed across ∼ 18 kpc scales with a resolution of ∼ 1 kpc. About 78% of the CO(1-0) luminosity traces a galaxy-size rotating disk. However, after subtracting the emission due to such rotating disk, we detect with a S/N=20 a residual emission in the central ∼ 4 kpc. Such residuals may trace a low velocity (v LOS = 170 km s −1 ) outflow. We compare the momentum rate ( P) and kinetic power ( E) of such putative molecular outflow with that of the X-ray UFO and find P mol / P U FO ∼ 0.4 and E mol / E U FO ∼ 4 · 10 −3 . This result is at odds with the energy-conserving scenario suggested by the large momentum boosts measured in some other molecular outflows. An alternative interpretation of the residual CO emission would be a compact rotating structure, distinct from the main disk, which would be a factor of ∼ 10 − 100 more extended and massive than typical circumnuclear disks revealed in Seyferts. In conclusion, in both scenarios, our results rule out the hypothesis of a momentum-boosted molecular outflow in this AGN, despite the presence of a powerful X-ray UFO.

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“…Such comparisons have now been performed for several additional sources (e.g. Mizumoto et al 2019b). How the AGN outflow travels have been studied in both the observational and theoretical viewpoint (e.g.…”

Section: Impact On Agn Feedbackmentioning

confidence: 99%

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

Mizumoto

Nomura

Done

et al. 2021

Monthly Notices of the Royal Astronomical Society

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UltraFast Outflows (UFO) are observed in some active galactic nuclei (AGN), with blueshifted and highly ionised Fe-K absorption features. AGN typically have a UV bright accretion flow, so UV line driving is an obvious candidate for launching these winds. However this mechanism requires material with UV opacity, in apparent conflict with the observed high ionisation state of the wind. In this paper we synthesise the X-ray energy spectra resulting from different lines of sight through a state of the art radiation hydrodynamics UV line driven disc wind simulation. We demonstrate that there are some lines of sight which only intercept highly ionised and fast outflowing material. The cooler material required for the UV line driving acceleration is out of the line of sight, close to the disc, shielded from the X-rays by a failed wind. We fit these simulated wind spectra to data from the archetypal UFO source PG 1211+143 and show that they broadly reproduce the depth and velocity of the iron absorption lines seen. This directly demonstrates that UV line driving is a viable mechanism to launch even the fastest UFOs. We simulate microcalorimeter observations of this wind and show that their high energy resolution can resolve the detailed structure in the wind and recover the wind energetics when combined with models which correctly estimate the line formation radius of the wind. New data from microcalorimeters will pave the way for physical predictions of AGN wind feedback in cosmological simulations.

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Kinetic Energy Transfer from X-Ray Ultrafast Outflows to Millimeter/Submillimeter Cold Molecular Outflows in Seyfert Galaxies

Cited by 32 publications

References 42 publications

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

A Momentum-conserving Accretion Disk Wind in the Narrow-line Seyfert 1 I Zwicky 1

Testing the blast-wave AGN feedback scenario in MCG-03-58-007

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

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