Jet-related Excitation of the [C ii] Emission in the Active Galaxy NGC 4258 with SOFIA

Appleton, P. N.; Díaz-Santos, T.; Fadda, D.; Ogle, Patrick; Togi, Aditya; Lanz, Lauranne; Alatalo, Katherine; Fischer, C.; Guillard, P.

doi:10.3847/1538-4357/aaed2a

Cited by 21 publications

(28 citation statements)

References 75 publications

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“…Dissipation of the kinetic energy of shocks and outflows can also have important consequences on the [C ii] emission, as theoretically explored by Lesaffre et al (2013). [C ii]/FIR ratios of 3-7% are detected in between merging galaxies (Appleton et al 2013;Peterson et al 2018) and locally within galaxies (Appleton et al 2018). On the global scale, the radio galaxy 3C 326 emits around 3% of FIR in [C ii] line for which jet-driven turbulence is likely responsible (Guillard et al 2015).…”

Section: Resultsmentioning

confidence: 99%

The Close AGN Reference Survey (CARS)

Smirnova-Pinchukova

Busch

Appleton

et al. 2019

A&A

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The [C II]λ158 μm line is one of the strongest far-infrared (FIR) lines and an important coolant in the interstellar medium of galaxies that is accessible out to high redshifts. The excitation of [C II] is complex and can best be studied in detail at low redshifts. Here we report the discovery of the highest global [C II] excess with respect to the FIR luminosity in the nearby AGN host galaxy HE 1353−1917. This galaxy is exceptional among a sample of five targets because the AGN ionization cone and radio jet directly intercept the cold galactic disk. As a consequence, a massive multiphase gas outflow on kiloparsec scales is embedded in an extended narrow-line region. Because HE 1353−1917 is distinguished by these special properties from our four bright AGN, we propose that a global [C II] excess in AGN host galaxies could be a direct signature of a multiphase AGN-driven outflow with a high mass-loading factor.

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Section: Resultsmentioning

confidence: 99%

The Close AGN Reference Survey (CARS)

Smirnova-Pinchukova

Busch

Appleton

et al. 2019

A&A

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“…Given the potential importance of feedback -the selfregulating gas cycle through which galaxies and AGN limit their own growth -it is important to understand what processes drive feedback and how the energy and momentum from young stellar populations and AGN is distributed and dissipated within the phases of the ISM and CGM (see, e.g., Guillard et al 2015;Gray & Scannapieco 2017;Appleton et al 2018;Buie et al 2018, and references therein). Understanding how the energy and momentum is distributed in bulk flows versus turbulence in gas, for example, provides insights into how feedback actually works in regulating galaxy and black hole growth.…”

Section: Introductionmentioning

confidence: 99%

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

Lehnert

Yang

Emonts

et al. 2020

A&A

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We present ALMA observations of hydrogen fluoride, HF J = 1–0, water, H2O (220–211), and the 1.2 THz rest-frame continuum emission from the z = 4.7 system BR 1202-0725. System BR 1202-0725 is a galaxy group consisting of a quasi-stellar object (QSO), a sub-millimeter galaxy (SMG), and a pair of Lyα emitters. We detected HF in emission in the QSO and possibly in absorption in the SMG, while water was detected in emission in both the QSO and the SMG. The QSO is the most luminous HF J = 1–0 emitter that has yet been found and has the same ratio of HF emission-line to infrared luminosity, LHF/LIR, as a small sample of local active galactic nuclei and the Orion Bar. This consistency covers about ten orders of magnitude in LIR. Based on the conclusions of a study of HF emission in the Orion Bar and simple radiative transfer modeling, the HF emission in the QSO is excited either by collisions with electrons (and H2) in molecular plasmas irradiated by the AGN and intense star formation, or predominately by collisions with H2, with a modest contribution from electrons, in a relatively high temperature (∼120 K), dense (∼105 cm−3) medium. The high density of electrons necessary to collisionally excite the HF J = 1–0 line can be supplied in sufficient quantities by the estimated column density of C+. Although HF should be an excellent tracer of molecular outflows, we found no strong kinematic evidence for outflows in HF in either the QSO or the SMG. From a putative absorption feature in HF observed against the continuum emission from the SMG, we conducted a bootstrap analysis to estimate an upper limit on the outflow rate, Ṁoutflow ≲ 45 M⊙ yr−1. This result implies that the ratio of the molecular outflow rate to the star formation rate is Ṁoutflow/SFR ≲ 5% for the SMG. Both the QSO and the SMG are among the most luminous H2O (220–211) emitters currently known and are found to lie along the same relationship between LH2O (220 − 211)/LIR and LIR as a large sample of local and high-redshift star-forming galaxies. The kinematics of the H2O (220–211) line in the SMG is consistent with a rotating disk as found previously but the line profile appears broader than other molecular lines, with a full width at half maximum of ∼1020 km s−1. The broadness of the line, which is similar to the width of a much lower resolution observation of CO(2-1), may suggest that either the gas on large scales (≳4 kpc) is significantly more disturbed and turbulent due either to interactions and mass exchange with the other members of the group, or to the dissipation of the energy of the intense star formation, or both. Overall however, the lack of significant molecular outflows in either source may imply that much of the energy from the intense star formation and active galactic nucleus in this pair is being dissipated in their interstellar media.

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“…We present the first X-ray detection of this jet-like structure using archival Chandra data. The radio continuum structure is remarkably similar to the ghostly counter-arms in the nearby galaxy NGC 4258 (Appleton et al 2018). In NGC 4258, about 40% of the [C II] emission in the central region comes from molecular gas excited by shocks and turbulence due to the jet propagating near the plane of the disk.…”

Section: Introductionmentioning

confidence: 67%

“…Such observations of shock-heated intergalactic warm H 2 also exhibit very broad [C II] line widths (400-600 km s −1 ) and unusually high [C II]/FIR and [C II]/PAH ratios. Models of warm molecular gas shocks (Appleton et al 2017) (Appleton et al 2018). The gas was found to correlate not only with warm mid-IR H 2 emission but also with soft X-ray emission relating to the activity of the jet in the inner regions of the galaxy.…”

Section: Introductionmentioning

confidence: 97%

[C ii] and CO Emission along the Bar and Counter-arms of NGC 7479*

Fadda

Laine

Appleton

2021

ApJ

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We present new SOFIA [C II] and ALMA CO J=1→0 observations of the nearby asymmetric barred spiral galaxy NGC 7479. The data, which cover the whole bar of the galaxy and the counter-arms visible in the radio continuum, are analyzed in conjunction with a wealth of existing visible, infrared, radio, and X-ray data. As in most normal galaxies, the [C II] emission is generally consistent with emission from cooling gas excited by photoelectric heating in photodissociation regions. However, anomalously high [C II]/CO ratios are seen at the two ends of the counterarms. Both ends show shell-like structures, possibly bubbles, in Hα emission. In addition, the southern end has [C II]-to-infrared emission ratios inconsistent with normal star formation. Because there is little H I emission at this location, the [C II] emission probably originates in warm shocked molecular gas heated by the interaction of the radio jet forming the counter-arms with the interstellar medium in the galaxy. At two other locations, the high [C II]/CO ratios provide evidence for the existence of patches of CO-dark molecular gas. The [C II] and CO observations also reveal resolved velocity components along the bar. In particular, the CO emission can be separated into two components associated with gas along the leading edge of the bar and gas trailing the bar. The trailing gas component that amounts to approximately 40% of the gas around the bar region may be related to a minor merger.Unified Astronomy Thesaurus concepts: Barred spiral galaxies (136); Infrared galaxies (790); Molecular gas (1073)

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Jet-related Excitation of the [C ii] Emission in the Active Galaxy NGC 4258 with SOFIA

Cited by 21 publications

References 75 publications

The Close AGN Reference Survey (CARS)

The Close AGN Reference Survey (CARS)

Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7

[C ii] and CO Emission along the Bar and Counter-arms of NGC 7479*

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Jet-related Excitation of the [C ii] Emission in the Active Galaxy NGC 4258 with SOFIA

Cited by 21 publications

References 75 publications

The Close AGN Reference Survey (CARS)

The Close AGN Reference Survey (CARS)

Etching glass in the early Universe: Luminous HF and H2O emission in a QSO-SMG pair at z = 4.7

[C ii] and CO Emission along the Bar and Counter-arms of NGC 7479*

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Etching glass in the early Universe: Luminous HF and H₂O emission in a QSO-SMG pair at z = 4.7