Extended X-Ray Emission in the H I Cavity of NGC 4151: Galaxy-Scale Active Galactic Nucleus Feedback?

Wang, Junfeng; Fabbiano, G.; Risaliti, G.; Elvis, M.; Mundell, C. G.; Dumas, G.; Schinnerer, E.; Zezas, A.

doi:10.1088/2041-8205/719/2/l208

Cited by 42 publications

(35 citation statements)

References 49 publications

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“…The "prototypical" Seyfert 1 galaxy, NGC 4151, occupies the most extreme position in the lower right quadrant. There is evidence, however, that the extended NLR in NGC 4151 was ionized when the central source was significantly more luminous than at present (e.g.. Schulz & Komossa 1993;Wang et al 2010). Hence, there may be a relatively large contribution from low density gas which would have the effect of reducing R O3 .…”

Section: One Caveat Regarding Estimates Of Reddening Based On the [O ...mentioning

confidence: 92%

Multi-Wavelength Probes of Obscuration Toward the Narrow-Line Region in Seyfert Galaxies

Kraemer¹,

Schmitt²,

Crenshaw³

et al. 2011

ApJ

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We present a study of reddening and absorption towards the Narrow Line Regions (NLR) in active galactic nuclei (AGN) selected from the Revised Shapley-Ames, 12µm, and Swift/Burst Alert Telescope samples. For the sources in host galaxies with inclinations of b/a > 0.5, we find that mean ratio of [O III] λ5007, from ground-based observations, and [O IV] 28.59µm, from Spitzer/Infrared Spectrograph observations, is a factor of 2 lower in Seyfert 2s than Seyfert 1s. The combination of low [O III]/[O IV] and [O III] λ4363/λ5007 ratios in Seyfert 2s suggests more extinction of emission from the NLR than in Seyfert 1s. Similar column densities of dusty gas, N H ∼ several × 10 21 cm −2 , can account for the suppression of both [O III] λ5007 and [O III] λ4363, as compared to those observed in Seyfert 1s. Also, we find that the X-ray line O VII λ22.1Å is weaker in Seyfert 2s, consistent with absorption by the same gas that reddens the optical emission. Using a Hubble Space Telescope/Space Telescope Imaging Spectrograph slitless spectrum of the Seyfert 1 galaxy NGC 4151, we estimate that only ∼ 30% of the [O III] λ5007 comes from within 30 pc of the central source, which is insufficient to account for the low [O III]/[O IV] ratios in Seyfert

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Section: One Caveat Regarding Estimates Of Reddening Based On the [O ...mentioning

confidence: 92%

Multi-Wavelength Probes of Obscuration Toward the Narrow-Line Region in Seyfert Galaxies

Kraemer¹,

Schmitt²,

Crenshaw³

et al. 2011

ApJ

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“…For comparison, we concentrate on their measured radial velocity centroids; the channel maps can be misleading because the NLR consists of large individual clouds of ionized gas with high velocity dispersions on the order of hundreds of km s −1 (Hutchings et al 1999;Das et al 2005), and each velocity channel samples not only clouds that have a velocity centroid in that channel, but also the velocity wings from a number of other clouds. Based on the velocity centroids, we prefer our model because we can clearly see the turnover from acceleration to deceleration in the STIS data (Das et al 2005, Figure 1c Using high-resolution X-ray imaging with the Chandra X-ray Observatory (CXO), Wang et al (2010Wang et al ( , 2011a found soft X-ray emission coincident with the optical NLR and extending out to over 1 kpc from the nucleus. They concluded that the soft X-ray gas was likely photoionized and calculatedṀ out ≈ 2 M ⊙ yr −1 and L KE ≈ 1.7 ×10 41 erg s −1 , indicating yet another important component of feedback in more highly ionized gas.…”

Section: Storchi-bergmann Et Al (2010) Present a Kinematic Model Of mentioning

confidence: 99%

Feedback From Mass Outflows in Nearby Active Galactic Nuclei. Ii. Outflows in the Narrow-Line Region of NGC 4151

Crenshaw

Fischer

Kraemer

et al. 2015

ApJ

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We present a detailed study of AGN feedback in the narrow-line region (NLR) of the Seyfert 1 galaxy NGC 4151. We illustrate the data and techniques needed to determine the mass outflow rate (Ṁ out ) and kinetic luminosity (L KE ) of the outflowing ionized gas as a function of position in the NLR. We find thatṀ out peaks at a value of 3.0 M ⊙ yr −1 at a distance of 70 pc from the central supermassive black hole (SMBH), which is about 10 times the outflow rate coming from inside 13 pc, and 230 times the mass accretion rate inferred from the bolometric luminosity of NGC 4151. Thus, most of the outflow must arise from "in situ" acceleration of ambient gas throughout the NLR. L KE peaks at 90 pc and drops rapidly thereafter, indicating that most of the kinetic energy is deposited within about 100 pc from the SMBH. Both values exceed theṀ out and L KE determined for the UV/X-ray absorber outflows in NGC 4151, indicating the importance of NLR outflows in providing feedback on scales where circumnuclear star formation and bulge growth occur.

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“…For the region outside, we would need a further consideration, but the clouds there could belong to a different episode of acceleration, further in the past. Wang et al (2010) identified an extended soft-X-ray emission in NGC4151 at ∼10 4 light years (a few kpc) from the nucleus. Based on its high surface brightness, they infer that this could be due to an episodic outburst of the nucleus which occurred ∼10 4 −10 5 years ago.…”

Section: "Agn Big Bang" -Episodic Accelerationmentioning

confidence: 94%

Velocity-inverted three-dimensional distribution of the gas clouds in the Type 2 AGN NGC1068

Miyauchi,

Kishimoto

2020

Preprint

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Spatially-resolved velocity maps at high resolutions of 1-10 pc are becoming available for many nearby AGNs in both optical/infrared atomic emission lines and sub-mm molecular lines. For the former, it has been known that a linear relationship appears to exist between the velocity of the ionized gas clouds and the distance from the nucleus in the inner ∼100 pc region, where these clouds are outflowing. Here we demonstrate that, in such a case, we can actually derive the three-dimensional (3D) geometrical distribution of the clouds directly from the velocity map. Revisiting such a velocity map taken by HST for the prototypical Type 2 AGN NGC1068, we implement the visualization of the 3D distribution derived from the map, and show that this inner narrow-line region has indeed a hollow-cone structure, consistent with previous modeling results. Quite possibly, this is the outer extended part of the polar elongated dusty material seen in the recent mid-IR interferometry at pc scale. Conversely, the latter small-scale geometry is inferred to have a hollow-cone outflowing structure as the inward extension of the derived 3D distribution above. The AGN obscuring "torus" is argued to be the inner optically thick part of this hollow-cone outflow, and its shadowed side would probably be associated with the molecular outflow seen in certain sub-mm lines. We discuss the nature of the linear velocity field, which could be from an episodic acceleration that had occurred ∼10 5 years ago.

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Extended X-Ray Emission in the H I Cavity of NGC 4151: Galaxy-Scale Active Galactic Nucleus Feedback?

Cited by 42 publications

References 49 publications

Multi-Wavelength Probes of Obscuration Toward the Narrow-Line Region in Seyfert Galaxies

Multi-Wavelength Probes of Obscuration Toward the Narrow-Line Region in Seyfert Galaxies

Feedback From Mass Outflows in Nearby Active Galactic Nuclei. Ii. Outflows in the Narrow-Line Region of NGC 4151

Velocity-inverted three-dimensional distribution of the gas clouds in the Type 2 AGN NGC1068

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