Magnetic interaction of jets and molecular clouds in NGC 4258

Krause, M.; Fendt, Christian; Neininger, N.

doi:10.1051/0004-6361:20066445

Cited by 26 publications

(37 citation statements)

References 46 publications

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“…Finally, it is also possible that the magnetic field created by the expanding, probably relativistic jet plays a role in accumulating molecular clouds towards its edges (e.g. by ambipolar diffusion, as proposed by Krause et al 2007 for NGC 4258).…”

Section: Under-luminous Co In the Ionisation Conementioning

confidence: 96%

AGN feedback in the nucleus of M 51

Schinnerer

García‐Burillo

Bigiel

et al. 2016

A&A

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AGN feedback is invoked as one of the most relevant mechanisms that shape the evolution of galaxies. Our goal is to understand the interplay between AGN feedback and the interstellar medium in M51, a nearby spiral galaxy with a modest AGN and a kpcscale radio jet expanding through the disc of the galaxy. For that purpose, we combine molecular gas observations in the CO(1-0) and HCN(1-0) lines from the Plateau de Bure interferometer with archival radio, X-ray, and optical data. We show that there is a significant scarcity of CO emission in the ionisation cone, while molecular gas emission tends to accumulate towards the edges of the cone. The distribution and kinematics of CO and HCN line emission reveal AGN feedback effects out to r ∼ 500 pc, covering the whole extent of the radio jet, with complex kinematics in the molecular gas which displays strong local variations. We propose that this is the result of the almost coplanar jet pushing on molecular gas in different directions as it expands; the effects are more pronounced in HCN than in CO emission, probably as the result of radiative shocks. Following previous interpretation of the redshifted molecular line in the central 5 as caused by a molecular outflow, we estimate the outflow rates to beṀ H 2 ∼ 0.9 M /yr andṀ dense ∼ 0.6 M /yr, which are comparable to the molecular inflow rates (∼1 M /yr); gas inflow and AGN feedback could be mutually regulated processes. The agreement with findings in other nearby radio galaxies suggests that this is not an isolated case, and probably the paradigm of AGN feedback through radio jets, at least for galaxies hosting low-luminosity active nuclei.

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Section: Under-luminous Co In the Ionisation Conementioning

confidence: 96%

AGN feedback in the nucleus of M 51

Schinnerer

García‐Burillo

Bigiel

et al. 2016

A&A

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“…Can we estimate the total mass flow rate in the filament? From an analysis of the faint CO emission seen associated faintly with the filament (Krause et al 2007), we measure a CO 1-0 line integral ΣS dV = 110 ± 10 Jy km s −1 . For D = 7.3 Mpc and assuming a Galactic value for X CO , we find an H 2 mass of 6×10 7 M .…”

Section: Regionmentioning

confidence: 99%

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

Appleton

Díaz-Santos

Fadda

et al. 2018

ApJ

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We detect widespread [C II] 157.7 µm emission from the inner 5 kpc of the active galaxy NGC 4258 with the SOFIA integral field spectrometer FIFI-LS. The emission is found associated with warm H 2 , distributed along and beyond the end of southern jet, in a zone known to contain shock-excited optical filaments. It is also associated with soft X-ray hot-spots, which are the counterparts of the "anomalous radio arms" of NGC 4258, and a 1 kpc-long filament on the minor axis of the galaxy which contains young star clusters. Palomar-CWI Hα integral field spectroscopy shows that the filament exhibits non-circular motions within NGC 4258. Many of the [C II] profiles are very broad, with the highest line width, 455 km s −1 , observed at the position of the southern jet bow-shock. Abnormally high ratios of L([C II])/L(FIR) and L([C II])/L(PAH7.7 µm) are found along and beyond the southern jet and in the X-ray hotspots. These are the same regions that exhibit unusually large intrinsic [C II] line widths. This suggests that the [C II] traces warm molecular gas in shocks and turbulence associated with the jet. We estimate that as much as 40% (3.8 × 10 39 erg s −1 ) of the total [C II] luminosity from the inner 5 kpc of NGC 4258 arises in shocks and turbulence (< 1% bolometric luminosity from the active nucleus), the rest being consistent with [C II] excitation associated with star formation. We propose that the highly-inclined jet is colliding with, and being deflected around, dense irregularities in a thick disk, leading to significant energy dissipation over a wide area of the galaxy.

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“…The inner radio is launched perpendicular to that disk (Herrnstein et al 1997), although on large spatial scales three helical braids of jets can be disentangled spectroscopically (Cecil et al 1992). The exact interpretation of the large-scale kinematics is still unclear (Krause et al 2007). …”

Section: Observations Of Jets In Binary Systemsmentioning

confidence: 99%

Wobbling and Precessing Jets From Warped Disks in Binary Systems

Sheikhnezami

Fendt

2015

ApJ

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We present results of the first ever three-dimensional (3D) magnetohydrodynamic (MHD) simulations of the accretion-ejection structure. We investigate the 3D evolution of jets launched symmetrically from single stars but also jets from warped disks in binary systems. We have applied various model setups and tested them by simulating a stable and bipolar symmetric 3D structure from a single star-disk-jet system. Our reference simulation maintains a good axial symmetry and also a bipolar symmetry for more than 600 rotations of the inner disk confirming the quality of our model setup. We have then implemented a 3D gravitational potential (Roche potential) due by a companion star and run a variety of simulations with different binary separations and mass ratios. These simulations show typical 3D deviations from axial symmetry, such as jet inclination outside the Roche lobe or spiral arms forming in the accretion disk. In order to find indication for precession effects, we have also run an exemplary parameter setup, essentially governed by a small binary separation of only 200 inner disk radii. This simulation shows strong indication that we observe the onset of a jet precession caused by the wobbling of the jet launching disk. We estimate the opening angle of the precession cone defined by the lateral motion of the the jet axis of about 4 degree after about 5000 dynamical time steps.

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Magnetic interaction of jets and molecular clouds in NGC 4258

Cited by 26 publications

References 46 publications

AGN feedback in the nucleus of M 51

AGN feedback in the nucleus of M 51

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

Wobbling and Precessing Jets From Warped Disks in Binary Systems

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