Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. IV. The Effects of Different Density Estimates on the Ionized Gas Masses and Outflow Rates

Revalski, Mitchell; Crenshaw, D. Michael; Rafelski, Marc; Kraemer, S. B.; Polack, Garrett E.; Falcão, Anna Trindade; Fischer, Travis C.; Meena, Beena; Martinez, Francisco; Schmitt, Henrique R.; Collins, Nicholas R.; Falcone, Julia

doi:10.3847/1538-4357/ac5f3d

Cited by 26 publications

(24 citation statements)

References 77 publications

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“…The same applies regarding the use of [S II] as an electron density estimator (Baron & Netzer 2019;Davies et al 2020;Riffel 2021;Revalski et al 2022).…”

Section: Mass-outflow Rates and Energeticsmentioning

confidence: 99%

“…Baron & Netzer (2019) suggest that the [S II] emission mainly arises close behind the ionization front, where most of the gas is neutral and n e is effectively lower (see also Figure 10 of Davies et al 2020). The bulk of the ionized gas is poorly traced by [S II], and using this line doublet as an electron density tracer may overestimate M out  (Revalski et al 2022). This systematic uncertainty would also affect the mass-outflow rates presented by Fiore et al (2017) and shown in Figure 10.…”

Section: Mass-outflow Rates and Energeticsmentioning

confidence: 99%

“…upper limits if sources other than AGN-driven outflows contribute to the local enhancement in gas dispersion (σ V,Hα ). The same applies regarding the use of [S II] as an electron density estimator (Baron & Netzer 2019;Davies et al 2020;Riffel 2021;Revalski et al 2022).…”

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confidence: 99%

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Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Molina

Wang

et al. 2022

ApJ

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We analyze Multi-Unit Spectroscopic Explorer observations of nine low-redshift (z < 0.1) Palomar-Green quasar host galaxies to investigate the spatial distribution and kinematics of the warm, ionized interstellar medium, with the goal of searching for and constraining the efficiency of active galactic nucleus (AGN) feedback. After separating the bright AGN from the starlight and nebular emission, we use pixel-wise, kpc-scale diagnostics to determine the underlying excitation mechanism of the line emission, and we measure the kinematics of the narrow-line region (NLR) to estimate the physical properties of the ionized outflows. The radial size of the NLR correlates with the AGN luminosity, reaching scales of ∼5 kpc and beyond. The geometry of the NLR is well-represented by a projected biconical structure, suggesting that the AGN radiation preferably escapes through the ionization cone. We find enhanced velocity dispersions (≳100 km s−1) traced by the Hα emission line in localized zones within the ionization cones. Interpreting these kinematic features as signatures of interaction between an AGN-driven ionized gas outflow and the host galaxy interstellar medium, we derive mass-outflow rates of ∼0.008–1.6 M ⊙ yr−1 and kinetic injection rates of ∼1039–1042 erg s−1, which yield extremely low coupling efficiencies of ≲10−3. These findings add to the growing body of recent observational evidence that AGN feedback is highly ineffective in the host galaxies of nearby AGNs.

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“…The same applies regarding the use of [S II] as an electron density estimator (Baron & Netzer 2019;Davies et al 2020;Riffel 2021;Revalski et al 2022).…”

Section: Mass-outflow Rates and Energeticsmentioning

confidence: 99%

Section: Mass-outflow Rates and Energeticsmentioning

confidence: 99%

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Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Molina

Wang

et al. 2022

ApJ

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“…The nuclear sphere of an AGN has a complex gas environment (e.g., Revalski et al 2022). We examine here how the gas environment affects the radiation behavior of an IKN.…”

Section: The Influence Of Gas Density In a Nuclear Spherementioning

confidence: 99%

Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei

Ren

Chen

Wang

et al. 2022

ApJL

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We investigate the dynamics and electromagnetic (EM) signatures of neutron star–neutron star (NS–NS) or neutron star–black hole (NS–BH) merger ejecta that occur in the accretion disk of an active galactic nucleus (AGN). We find that the interaction between ejecta and disk gas leads to important effects on the dynamics and radiation. We show five stages of the ejecta dynamics: gravitational slowing down, coasting, Sedov–Taylor deceleration in the disk, reacceleration after the breakout from the disk surface, and momentum-conserved snowplow phase. Meanwhile, the radiation from the ejecta is so bright that its typical peak luminosity reaches a few times 1043–1044 erg s−1. Since most of the radiation energy has converted from the kinetic energy of merger ejecta, we call such an explosive phenomenon an interacting kilonova (IKN). It should be emphasized that IKNe are very promising, bright EM counterparts to NS–NS/BH–NS merger events in AGN disks. The bright peak luminosity and long rising time (i.e., 10 to 20 days in UV bands, 30 to 50 days in optical bands, and 100 days to hundreds of days in IR bands) allow most survey telescopes to have ample time to detect an IKN. However, the peak brightness, peak time, and evolution pattern of the light curve of an IKN are similar to a superluminous supernova in a galactic nucleus and a tidal disruption event making it difficult to distinguish between them. But it also suggests that IKNe might have been present in recorded AGN transients.

show abstract

“…The nuclear sphere of AGN has a complex gas environment (e.g., Revalski et al 2022). We examine here how the gas environment affects the radiation behavior of an IKN.…”

Section: The Influence Of Gas Density In a Nuclear Spherementioning

confidence: 99%

Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei

Jia¹,

Chen²,

Wang³

et al. 2022

Preprint

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We investigate the dynamics and electromagnetic (EM) signatures of neutron star-neutron star (NS-NS) or neutron star-black hole (NS-BH) merger ejecta that occurs in the accretion disk of an active galactic nucleus (AGN). We find that the interaction between ejecta and disk gas leads to important effects on the dynamics and radiation. We show five stages of the ejecta dynamics: gravitational slowing down, coasting, Sedov-Taylor deceleration in the disk, re-acceleration after the breakout from the disk surface, and momentum-conserved snowplow phase. Meanwhile, the radiation from the ejecta is so bright that its typical peak luminosity reaches a few times 10 43 − 10 44 erg s −1 . Since most of the radiation energy has converted from the kinetic energy of merger ejecta, we call such an explosive phenomenon an interacting kilonova (IKN). It should be emphasized that IKNe are very promising, bright EM counterparts to NS-NS/BH-NS merger events in AGN disks. The bright peak luminosity and long rising time (i.e., ten to twenty days in UV bands, thirty to fifty days in optical bands, and one hundred days to hundreds of days in IR bands) allow most survey telescopes to have ample time to detect an IKN. However, the peak brightness, peak time, and evolution pattern of the light curve of an IKN are similar to a superluminous supernova in a galactic nucleus and a tidal disruption event making it difficult to distinguish between them. But it also suggests that IKNe might have been present in recorded AGN transients.

show abstract

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. IV. The Effects of Different Density Estimates on the Ionized Gas Masses and Outflow Rates

Cited by 26 publications

References 77 publications

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Ionized Outflows in Nearby Quasars Are Poorly Coupled to Their Host Galaxies

Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei

Interacting Kilonovae: Long-lasting Electromagnetic Counterparts to Binary Mergers in the Accretion Disks of Active Galactic Nuclei

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