A Dissection of Spatially Resolved AGN Feedback across the Electromagnetic Spectrum

Fischer, Travis C.; Smith, Krista Lynne; Kraemer, Steve; Schmitt, H. R.; Crenshaw, D. Michael; Koss, Michael; Mushotzky, R. F.; Larson, Kirsten L.; Vivian, U; Rigby, J. Keith

doi:10.3847/1538-4357/ab55e3

Cited by 18 publications

(26 citation statements)

References 69 publications

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“…The radio emission is spatially located in the region of the blue-shifted part of the outflow. In AGN driven outflows there is often a similar orientation of radio emission and outflow as we see here in NGC 5077, but not a perfect spatial correlation (Müller-Sánchez et al 2011, Fischer et al 2019. The radio emission is in some cases associated with a jet that is interacting with the interstellar medium and transferring angular momentum to the gas to power the AGN outflow.…”

Section: Nuclear Gas Outflowmentioning

confidence: 52%

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External gas accretion provides a fresh gas supply to the active S0 galaxy NGC 5077

Raimundo

2021

A&A

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In early-type galaxies, externally accreted gas is thought to be the main source of gas replenishment at late times. We use MUSE integral field spectroscopy data to study the active S0 galaxy NGC 5077, which is known to have disturbed dynamics that are indicative of a past external interaction. We confirm the presence of a stellar kinematically distinct core with a diameter of 2.8 kpc that is counter-rotating with respect to the main stellar body of the galaxy. We find that the counter-rotating core consists of an old stellar population that is not significantly different from the rest of the galaxy. The ionised gas is strongly warped and extends out to 6.5 kpc in the polar direction and in a filamentary structure. The gas dynamics is complex, with significant changes in the position angle as a function of radius. The ionised gas line ratios are consistent with LINER excitation by the active galactic nucleus, both in the nucleus and at kiloparsec scales. We discover a nuclear outflow with projected velocity V ∼ 400 km s−1, consistent with a hollow outflow cone intersecting the plane of the sky. The properties of the misaligned gas match predictions from numerical simulations of misaligned gas infall after a gas-rich merger. The warp and change in the gas orientation as a function of radius are consistent with gas relaxation due to stellar torques; these are stronger at small radii where the gas aligns faster than in the outer regions, driving gas to the nucleus. The stellar and gas dynamics indicate that NGC 5077 has had at least two external interactions, one that resulted in the formation of the counter-rotating core, followed by the second, late-time external gas accretion. NGC 5077 illustrates the importance of external interactions in the replenishment of the galaxy gas reservoir and the nuclear gas content available for black hole fuelling.

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Section: Nuclear Gas Outflowmentioning

confidence: 52%

“…In the case of NGC 5077, the radio emission may be caused by synchrotron emission from relativistic particles that are accelerated in the shocks caused by the AGN outflow (e.g. Zakamska & Greene 2014, Fischer et al 2019).…”

Section: Nuclear Gas Outflowmentioning

confidence: 99%

External gas accretion provides a fresh gas supply to the active S0 galaxy NGC 5077

Raimundo

2021

A&A

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“…However, the presence of disturbed gas at larger radial distances (F2018), suggests that the AGN have an effect outside the outflow regions. One possibility is that this is the result of X-ray winds, which may form from thermal expansion of the [O III] gas (Fischer et al 2019;Kraemer et al 2020). We are currently exploring this scenario (Trindade Falcão et al, in preparation).…”

Section: Discussionmentioning

confidence: 99%

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

Falcão

Kraemer

Fischer

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use Hubble Space Telescope (HST)/ Space Telescope Imaging Spectrograph (STIS) long-slit G430M and G750M spectra to analyse the extended [O III] λ5007 emission in a sample of twelve nearby (z >0.12) luminous (Lbol > 1.6 × 1045 erg s−1) QSO2s. The purpose of the study is to determine the properties of the mass outflows of ionised gas and their role in AGN feedback. We measure fluxes and velocities as functions of radial distances. Using Cloudy models and ionising luminosities derived from [O III] λ5007, we are able to estimate the densities for the emission-line gas. From these results, we derive masses of [O III]-emitting gas, mass outflow rates, kinetic energies, kinetic luminosities, momenta and momentum flow rates as a function of radial distance for each of the targets. For the sample, masses are several times 103M⊙ − 107M⊙ and peak outflow rates are 9.3 × 10−3M⊙ yr−1 to 10.3 M⊙ yr−1. The peak kinetic luminosities are 3.4 × 10−8 to 4.9 × 10−4 of the bolometric luminosity, which does not approach the 5.0 × 10−3 - 5.0 × 10−2 range required by some models for efficient feedback. For Mrk 34, which has the largest kinetic luminosity of our sample, in order to produce efficient feedback there would have to be 10 times more [O III]-emitting gas than we detected at its position of maximum kinetic luminosity. Three targets show extended [O III] emission, but compact outflow regions. This may be due to different mass profiles or different evolutionary histories.

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“…We calculate the radial mass profiles of Mrk 477 and Mrk 34, which we use as inputs to our dynamical analysis described in Section 4. The radial mass distributions of Mrk 477 and Mrk 34 are determined using HST/Wide-Field Planetary Camera 3 (WFPC3) F814W images, employing the method described by Fischer et al (2019); specifically, we use Galfit version 3.0.5 (Peng et al 2002(Peng et al , 2010 to perform image decomposition to separate the galaxy/stellar light from the nuclear emission. We find that the best-fitting model is composed of two Sérsic components for Mrk 34 and three components for Mrk 477.…”

Section: The Radial Mass Profiles Of Mrk 477 and Mrk 34mentioning

confidence: 99%

“…If the disturbance of the [O III] gas (Fischer et al 2019) in Mrk 34 is due to interaction with an X-ray wind, we can assume that the wind is depositing kinetic energy into the [O III] gas, which suggests that X-ray wind and the [O III] gas may possess similar kinetic energy densities. Here we are assuming an 'ideal case' scenario, in which we ignore any sort of energy dissipation (e.g.…”

Section: Kinetic Energy Density Analysismentioning

confidence: 99%

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

Falcão

Kraemer

Fischer

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a dynamical study of the narrow-line regions in two nearby QSO2s. We construct dynamical models based on detailed photoionisation models of the emission-line gas, including the effects of internal dust, to apply to observations of large-scale outflows from these AGNs. We use Mrk 477 and Mrk 34 in order to test our models against recent HST STIS observations of [O III] emission-line kinematics, since these AGNs possess more energetic outflows than found in Seyfert galaxies. We find that the outflows within 500 pc are consistent with radiative acceleration of dusty gas, however the outflows in Mrk 34 are significantly more extended and may not be directly accelerated by radiation. We characterise the properties of X-ray winds found from the expansion of [O III]-emitting gas close to the black hole. We show that such winds possess the kinetic energy density to disturb [O III] gas at ∼ 1.8 kpc, and have sufficient energy to entrain the [O III] clouds at ∼ 1.2 kpc. Assuming that the X-ray wind possesses the same radial mass distribution as the [O III] gas, we find that the peak kinetic luminosity for this wind is 2 per cent of Mrk 34’s bolometric luminosity, which is in the 0.5 per cent - 5 per cent range required by some models for efficient feedback. Our work shows that, although the kinetic luminosity as measured from [O III]-emitting gas is frequently low, X-ray winds may provide more than one order of magnitude higher kinetic power.

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A Dissection of Spatially Resolved AGN Feedback across the Electromagnetic Spectrum

Cited by 18 publications

References 69 publications

External gas accretion provides a fresh gas supply to the active S0 galaxy NGC 5077

External gas accretion provides a fresh gas supply to the active S0 galaxy NGC 5077

Hubble Space Telescope observations of [O iii] emission in nearby QSO2s: physical properties of the ionized outflows

Hubble Space Telescope[O iii] emission-line kinematics in two nearby QSO2s: a case for X-ray feedback

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