Near-Infrared Spectroscopy of Nearby Seyfert Galaxies: Is There Evidence for Shock Excitation in Narrow-Line Regions?

Terao, Koki; Nagao, Tohru; Hashimoto, Tetsuya; Yanagisawa, K.; Matsuoka, Kenta; Toba, Yoshiki; Ikeda, Hiroyuki; Taniguchi, Yoshiaki

doi:10.3847/1538-4357/833/2/190

Cited by 16 publications

(13 citation statements)

References 108 publications

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“…As noted by others (Schlesinger et al 2009), we do not see any evidence for shock ionization in the outflow regions (see, e.g. Schlesinger et al 2009;Maksym et al 2016Maksym et al , 2017Terao et al 2016, and references therein for dis- cussions on shocks). Our composite models qualitatively agree with the IUE UV line ratios, indicating that we are likely encompassing a significant portion of the UV emitting gas in our models and resulting outflow rates.…”

Section: Model Comparison To the Observationssupporting

confidence: 74%

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†

Revalski

Crenshaw

Kraemer

et al. 2018

ApJ

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We present the first spatially resolved mass outflow rate measurements (Ṁ out ) of the optical emission line gas in the narrow line region (NLR) of a Seyfert 2 galaxy, Markarian 573. Using long slit spectra and [O III] imaging from the Hubble Space Telescope and Apache Point Observatory in conjunction with emission line diagnostics and Cloudy photoionization models, we find a peak outflow rate oḟ M out ≈ 3.4 ± 0.5 M ⊙ yr −1 at a distance of 210 pc from the central supermassive black hole (SMBH). The outflow extends to distances of 600 pc from the nucleus with a total mass and kinetic energy of M ≈ 2.2 × 10 6 M ⊙ and E ≈ 5.1 × 10 54 erg, revealing the outflows to be more energetic than those in the lower luminosity Seyfert 1 galaxy NGC 4151 (Crenshaw et al. 2015). The peak outflow rate is an order of magnitude larger than the mass accretion and nuclear outflow rates, indicating local in-situ acceleration of the circumnuclear NLR gas. We compare these results to global techniques that quantify an average outflow rate across the NLR, and find the latter are subject to larger uncertainties. These results indicate that spatially resolved observations are critical for probing AGN feedback on scales where circumnuclear star formation occurs.

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Section: Model Comparison To the Observationssupporting

confidence: 74%

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†

Revalski

Crenshaw

Kraemer

et al. 2018

ApJ

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“…In our 1.5 − 8.0 annular region, however, we find a thermal component that may be associated with fast shocks. This is not necessarily inconsistent with the Terao et al (2016) results, since nonradiative, fast shocks would not be observed in the optical/IR. The photoionization parameters from our best fits also provide constraints on the presence of highly ionized outflows, such as warm absorbers (WAs), in NGC 7212.…”

Section: Physical Modelsmentioning

confidence: 52%

Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

Jones

Fabbiano

Elvis

et al. 2020

ApJ

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Recent observations of nearby Compton thick (CT) active galactic nuclei (AGNs) with Chandra have resolved hard (> 3 keV) X-ray emission extending out from the central supermassive black hole to kiloparsec scales, challenging the long-held belief that the characteristic hard X-ray continuum and fluorescent Fe K lines originate in the inner ∼parsec due to the excitation of obscuring material. In this paper we present the results of the most recent Chandra ACIS-S observations of NGC 7212, a CT AGN in a compact group of interacting galaxies, with a total effective exposure of ∼150 ks. We find ∼20% of the observed emission is found outside of the central kiloparsec, with ∼17% associated with the soft X-rays, and ∼3% with hard X-ray continuum and Fe K line. This emission is extended both along the ionization cone and in the cross-cone direction up to ∼3.8 kpc scales. The spectrum of NGC 7212 is best represented by a mixture of thermal and photoionization models that indicate the presence of complex gas interactions. These observations are consistent with what is observed in other CT AGN (e.g., ESO 428−G014, NGC 1068), providing further evidence that this may be a common phenomenon. High-resolution observations of extended CT AGN provide an especially valuable environment for understanding how AGN feedback impacts host galaxies on galactic scales.

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“…Marconi et al 2000;Krajnović et al 2007). The sharp rise of the [Fe II]/[P II] ratio with apertures up to 1.25 (Krajnović et al 2007) suggests an increasingly dominating shock contribution (see Terao et al 2016). In addition, the high surface brightness of the 1−0 S (1) (Israel et al 1990 (Sturm et al 2002;Ogle et al 2010) is likewise characteristic for shock excitation and incompatible with the PDR models of Kaufman et al (2006) for any reasonable combination of density n • and radiation field G. At least the [S III] flux originates in a region less than 11 across, excluding emission from either the outer CND or the outflow.…”

Section: Shocked Molecular Gas In the Centermentioning

confidence: 97%

The outflow of gas from the Centaurus A circumnuclear disk

Israel

Guêsten

Meijerink

et al. 2017

A&A

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The physical state of the gas in the central 500 pc of NGC 5128 (the radio galaxy Centaurus A), was investigated using the finestructure lines of carbon [C I], [C II]; oxygen [O I], [O III], and nitrogen [N II], [N III] as well as the 12 CO(4−3) molecular line. The circumnuclear disk (CND) is traced by emission from dust and the neutral gas ([C I] and 12 CO). A gas outflow with a line-of-sight velocity of 60 km s −1 is evident in both lines. The [C I] emission from the CND is unusually strong with respect to that from CO. The center of the CND (R < 90 pc) is bright in [O I], [O III], and [C II]; [O I]λ63 µm emission dominates that of [C II] even though it is absorbed with optical depths τ = 1.0−1.5. The outflow is well-traced by the [N II] and [N III] lines and also seen in the [C II] and [O III] lines that peak in the center. Ionized gas densities are highest in the CND (about 100 cm −3) and low everywhere else. Neutral gas densities range from 4000 cm −3 (outflow, extended thin disk ETD) to 20 000 cm −3 (CND). The CND radiation field (G o ≈ 4) is weak compared to the ETD starburst field (G o ≈ 40). The outflow has a much stronger radiation field (G o = 130). The total mass of all the CND gas is 9.1 ± 0.9 × 10 7 M but the mass of the outflowing gas is only 15−30% of that. The outflow most likely originates from the shock-dominated CND cavity surrounding the central black hole. With a factor of three uncertainty, the mass outflow rate is ≈2 M yr −1 , a thousand times higher than the accretion rate of the black hole. Without replenishment, the CND will be depleted in 15−120 million years. However, the outflow velocity is well below the escape velocity.

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Near-Infrared Spectroscopy of Nearby Seyfert Galaxies: Is There Evidence for Shock Excitation in Narrow-Line Regions?

Cited by 16 publications

References 108 publications

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†

Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

The outflow of gas from the Centaurus A circumnuclear disk

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Near-Infrared Spectroscopy of Nearby Seyfert Galaxies: Is There Evidence for Shock Excitation in Narrow-Line Regions?

Cited by 16 publications

References 108 publications

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573∗ †

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573∗ †

Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission

The outflow of gas from the Centaurus A circumnuclear disk

Contact Info

Product

Resources

About

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†

Quantifying Feedback from Narrow Line Region Outflows in Nearby Active Galaxies. I. Spatially Resolved Mass Outflow Rates for the Seyfert 2 Galaxy Markarian 573^∗ ^†