ORCID Profile
0000-0002-5104-6434
Current Organisations
University of Tsukuba
,
Tsukuba Daigaku Keisan Kagaku Kenkyu Center
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Research Topics
In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
Astronomical and Space Sciences | Cosmology and Extragalactic Astronomy | Numerical Computation
ANZSRC Socio-Economic Objective (SEO)
Expanding Knowledge in the Physical Sciences | Expanding Knowledge in the Information and Computing Sciences |
Related Links
Publications
Jet-intracluster medium interaction in Hydra A - II. The effect of jet precession
Publisher: Oxford University Press (OUP)
Date: 15-02-2016
DOI: 10.1093/MNRAS/STW330
Erratum: Relativistic jet feedback in high-redshift galaxies I. Dynamics
Publisher: Oxford University Press (OUP)
Date: 14-07-2017
Stereo pairs in Astrophysics
Publisher: Springer Science and Business Media LLC
Date: 02-09-2012
Modelling observable signatures of jet-ISM interaction: thermal emission and gas kinematics
Publisher: Oxford University Press (OUP)
Date: 11-08-2022
Abstract: Relativistic jets are believed to have a substantial impact on the gas dynamics and evolution of the interstellar medium (ISM) of their host galaxies. In this paper, we aim to draw a link between the simulations and the observable signatures of jet-ISM interactions by analyzing the emission morphology and gas kinematics resulting from jet-induced shocks in simulated disc and spherical systems. We find that the jet-induced laterally expanding forward shock of the energy bubble sweeping through the ISM causes large-scale outflows, creating shocked emission and high-velocity dispersion in the entire nuclear regions (∼2 kpcs) of their hosts. The jetted systems exhibit larger velocity widths (& km s−1), broader Position-Velocity maps and distorted symmetry in the disc’s projected velocities than systems without a jet. We also investigate the above quantities at different inclination angles of the observer with respect to the galaxy. Jets inclined to the gas disc of its host are found to be confined for longer times, and consequently couple more strongly with the disc gas. This results in prominent shocked emission and high-velocity widths, not only along the jet’s path, but also in the regions perpendicular to them. Strong interaction of the jet with a gas disc can also distort its morphology. However, after the jets escape their initial confinement, the jet-disc coupling is weakened, thereby lowering the shocked emission and velocity widths.
Cosmic ray moderation of the thermal instability
Publisher: EDP Sciences
Date: 20-01-2005
Shock-multicloud interactions in galactic outflows - I. Cloud layers with lognormal density distributions
Publisher: Oxford University Press (OUP)
Date: 23-09-2020
Abstract: We report three-dimensional hydrodynamical simulations of shocks (${\\cal M_{\\rm shock}}\\ge 4$) interacting with fractal multicloud layers. The evolution of shock–multicloud systems consists of four stages: a shock-splitting phase in which reflected and refracted shocks are generated, a compression phase in which the forward shock compresses cloud material, an expansion phase triggered by internal heating and shock re-acceleration, and a mixing phase in which shear instabilities generate turbulence. We compare multicloud layers with narrow ($\\sigma _{\\rho }=1.9\\bar{\\rho }$) and wide ($\\sigma _{\\rho }=5.9\\bar{\\rho }$) lognormal density distributions characteristic of Mach ≈ 5 supersonic turbulence driven by solenoidal and compressive modes. Our simulations show that outflowing cloud material contains imprints of the density structure of their native environments. The dynamics and disruption of multicloud systems depend on the porosity and the number of cloudlets in the layers. ‘Solenoidal’ layers mix less, generate less turbulence, accelerate faster, and form a more coherent mixed-gas shell than the more porous ‘compressive’ layers. Similarly, multicloud systems with more cloudlets quench mixing via a shielding effect and enhance momentum transfer. Mass loading of diffuse mixed gas is efficient in all models, but direct dense gas entrainment is highly inefficient. Dense gas only survives in compressive clouds, but has low speeds. If normalized with respect to the shock-passage time, the evolution shows invariance for shock Mach numbers ≥10 and different cloud-generating seeds, and slightly weaker scaling for lower Mach numbers and thinner cloud layers. Multicloud systems also have better convergence properties than single-cloud systems, with a resolution of eight cells per cloud radius being sufficient to capture their overall dynamics.
Relativistic jet feedback in high-redshift galaxies - I. Dynamics
Publisher: Oxford University Press (OUP)
Date: 08-06-2016
Relativistic jet feedback - II. Relationship to gigahertz peak spectrum and compact steep spectrum radio galaxies
Publisher: Oxford University Press (OUP)
Date: 10-01-2018
DOI: 10.1093/MNRAS/STY070
The extent of ionization in simulations of radio-loud AGNs impacting kpc gas discs
Publisher: Oxford University Press (OUP)
Date: 28-01-2022
Abstract: We use the results of relativistic hydrodynamic simulations of jet-interstellar medium (ISM) interactions in a galaxy with a radio-loud AGN to quantify the extent of ionization in the central few kpcs of the gaseous galactic disc. We perform post-process radiative transfer of AGN radiation through the simulated gaseous jet-perturbed disc to estimate the extent of photo-ionization by the AGN with an incident luminosity of 1045 erg s−1. We also map the gas that is collisionally ionized due to shocks driven by the jet. The analysis was carried out for simulations with similar jet power (1045 erg s−1) but different jet orientations with respect to the gas disc. We find that the shocks from the jets can ionize a significant fraction (up to 33 ${{\\ \\rm per\\ cent}}$) of dense gas ($n\\gt 100\\, \\mathrm{cm^{-3}}$) in the disc, and that the jets clear out the central regions of gas for AGN radiation to penetrate to larger distances in the disc. Jets inclined towards the disc plane couple more strongly with the ISM and ionize a larger fraction of gas in the disc as compared to the vertical jet. However, similar to previous studies, we find that the AGN radiation is quickly absorbed by the outer layers of dense clouds in the disc, and is not able to substantially ionize the disc on a global scale. Thus, compared to jet–ISM interactions, we expect that photo-ionization by the AGN radiation only weakly affects the star-formation activity in the central regions of the galactic disc (≲ 1 kpc), although the jet-induced shocks can spread farther out.
RELATIVISTIC JET FEEDBACK IN EVOLVING GALAXIES
Publisher: American Astronomical Society
Date: 17-01-2011
Resolved simulations of jet–ISM interaction: Implications for gas dynamics and star formation
Publisher: Wiley
Date: 11-2021
Abstract: Relativistic jets can interact with the ambient gas distribution of the host galaxy, before breaking out to larger scales. In the past decade, several studies have simulated jet‐driven outflows to understand how they affect the nearby environment, and over what spatial and temporal scales such interactions occur. The simulations are able to capture the interaction of the jets with the turbulent clumpy interstellar medium and the resultant energetics of the gas. In this review, we summarize the results of such recent studies and discuss their implications on the evolution of the dynamics of the gas distribution and the star formation rate.
DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY
Publisher: American Astronomical Society
Date: 12-09-2012
How frequent are close supermassive binary black holes in powerful jet sources?
Publisher: Oxford University Press (OUP)
Date: 21-09-2018
MULTI-DIMENSIONAL SIMULATIONS OF THE EXPANDING SUPERNOVA REMNANT OF SN 1987A
Publisher: American Astronomical Society
Date: 07-10-2014
The Effects of Cosmic Rays on Interstellar Dynamics
Publisher: Springer Netherlands
Date: 2007
Outflows driven by quasars in high-redshift galaxies with radiation hydrodynamics
Publisher: Oxford University Press (OUP)
Date: 16-09-2016
Jet-induced molecular gas excitation and turbulence in the Teacup
Publisher: EDP Sciences
Date: 03-2023
DOI: 10.1051/0004-6361/202345964
Abstract: In order to investigate the impact of radio jets on the interstellar medium (ISM) of galaxies hosting active galactic nuclei (AGN), we present subarcsecond-resolution Atacama Large Millimeter/submillimeter Array (ALMA) CO(2-1) and CO(3-2) observations of the Teacup galaxy. This is a nearby ( D L = 388 Mpc) radio-quiet type-2 quasar (QSO2) with a compact radio jet ( P jet ≈ 10 43 erg s −1 ) that subtends a small angle from the molecular gas disc. Enhanced emission line widths perpendicular to the jet orientation have been reported for several nearby AGN for the ionised gas. For the molecular gas in the Teacup, not only do we find this enhancement in the velocity dispersion but also a higher brightness temperature ratio ( T 32 / T 21 ) perpendicular to the radio jet compared to the ratios found in the galaxy disc. Our results and the comparison with simulations suggest that the radio jet is compressing and accelerating the molecular gas, and driving a lateral outflow that shows enhanced velocity dispersion and higher gas excitation. These results provide further evidence that the coupling between the jet and the ISM is relevant to AGN feedback even in the case of radio-quiet galaxies.
A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). IV. Rapidly Growing (Super)Massive Black Holes in Extremely Radio-loud Galaxies
Publisher: American Astronomical Society
Date: 29-10-2021
Shock-multicloud interactions in galactic outflows - II. Radiative fractal clouds and cold gas thermodynamics
Publisher: Oxford University Press (OUP)
Date: 02-07-2021
Abstract: Galactic winds are crucial to the cosmic cycle of matter, transporting material out of the dense regions of galaxies. Observations show the coexistence of different temperature phases in such winds, which is not easy to explain. We present a set of 3D shock–multicloud simulations that account for radiative heating and cooling at temperatures between $10^2$ and $10^7\\, \\rm K$. The interplay between shock heating, dynamical instabilities, turbulence, and radiative heating and cooling creates a complex multiphase flow with a rain-like morphology. Cloud gas fragments and is continuously eroded, becoming efficiently mixed and mass loaded. The resulting warm mixed gas then cools down and precipitates into new dense cloudlets, which repeat the process. Thus, radiative cooling is able to sustain fast-moving dense gas by aiding condensation of gas from warm clouds and the hot wind. In the ensuing outflow, hot gas with temperatures ${\\gtrsim}10^6\\, \\rm K$ outruns the warm and cold phases, which reach thermal equilibrium near ${\\approx}10^4$ and ${\\approx}10^2\\, \\rm K$, respectively. Although the volume filling factor of hot gas is higher in the outflow, most of the mass is concentrated in dense gas cloudlets and filaments with these temperatures. More porous multicloud layers result in more vertically extended outflows, and dense gas is more efficiently produced in more compact layers. The cold phase is not accelerated by ram pressure, but, instead, precipitates from warm and mixed gas out of thermal equilibrium. This cycle can explain the presence of high-velocity H i gas with $N_{\\rm H\\, \\small {I}}=10^{19\\!-\\!21}\\, \\rm cm^{-2}$ and $\\Delta v_{{\\rm FWHM}}\\lesssim 37\\, \\rm km\\, s^{-1}$ in the Galactic Centre outflow.
ULTRAFAST OUTFLOWS: GALAXY-SCALE ACTIVE GALACTIC NUCLEUS FEEDBACK
Publisher: American Astronomical Society
Date: 04-01-2013
Jets blowing bubbles in the young radio galaxy 4C 31.04
Publisher: Oxford University Press (OUP)
Date: 23-01-2019
DOI: 10.1093/MNRAS/STZ233
Jet-intracluster medium interaction in Hydra A - I. Estimates of jet velocity from inner knots
Publisher: Oxford University Press (OUP)
Date: 29-08-2014
The jet–ISM interactions in IC 5063
Publisher: Oxford University Press (OUP)
Date: 22-01-2018
DOI: 10.1093/MNRAS/STY067
A COSMIC-RAY PRECURSOR MODEL FOR A BALMER-DOMINATED SHOCK IN TYCHO'S SUPERNOVA REMNANT
Publisher: American Astronomical Society
Date: 12-12-2008
Relating gas dynamics to star formation in the central region of the barred spiral galaxy NGC 613
Publisher: Oxford University Press (OUP)
Date: 07-2021
DOI: 10.1093/PASJ/PSAB060
Abstract: The barred spiral galaxy NGC 613 has a star-forming ring in the center, and near-infrared observations have previously shown that the star formation activity on the eastern and western sides of the ring is asymmetric. We examined the dynamics and physical state of the molecular gas in the ring using high-resolution (∼15 pc) 12CO(1–0), 12CO(3–2), and 13CO(1–0) observations with ALMA. Using a dendrogram, we identified 111 molecular clouds in the bar and ring, and found that the virial parameter (αvir) gradually decreases (αvir & 2) toward the confluence of the northern bar and eastern ring, while the virial parameter is large (αvir & 2) around the corresponding confluence in the western side of the ring. A non-LTE analysis using RADEX showed that the temperature and density of the molecular gas increase downstream of the eastern point of confluence, whereas they change irregularly on the western side. The star formation efficiency is (1.7 ± 0.2) × 10−8 yr−1 in the eastern side of the ring, which is substantially higher than the (0.9 ± 0.3) × 10−8 yr−1 for the western side of the ring. Position–velocity diagrams show that the relative velocity of the gas between the bar and the ring is ∼70 km s−1 in the east, while it reaches ∼170 km s−1 in the west. We suggest that the star formation activity in the central region of NGC 613 depends strongly on the relative velocity of the gas between the bar and the ring.
Searching for signs of jet-driven negative feedback in the nearby radio galaxy UGC 05771
Publisher: Oxford University Press (OUP)
Date: 05-09-2019
Abstract: Hydrodynamical simulations predict that the jets of young radio sources can inhibit star formation in their host galaxies by injecting heat and turbulence into the interstellar medium (ISM). To investigate jet–ISM interactions in a galaxy with a young radio source, we have carried out a multiwavelength study of the z = 0.025 Compact Steep Spectrum radio source hosted by the early-type galaxy UGC 05771. Using Keck/OSIRIS observations, we detected H2 1–0 S(1) and [Fe ii] emission at radii of 100s of parsecs, which traces shocked molecular and ionized gas being accelerated outwards by the jets to low velocities, creating a ‘stalling wind’. At kpc radii, we detected shocked ionized gas using observations from the CALIFA survey, covering an area much larger than the pc-scale radio source. We found that existing interferometric radio observations fail to recover a large fraction of the source’s total flux, indicating the likely existence of jet plasma on kpc scales, which is consistent with the extent of shocked gas in the host galaxy. To investigate the star formation efficiency in UGC 05771, we obtained IRAM CO observations to analyse the molecular gas properties. We found that UGC 05771 sits below the Kennicutt–Schmidt relation, although we were unable to definitively conclude if direct interactions from the jets are inhibiting star formation. This result shows that jets may be important in regulating star formation in the host galaxies of compact radio sources.
Galaxy-scale AGN feedback - theory
Publisher: Wiley
Date: 02-2016
Abstract: Powerful relativistic jets in radio galaxies are capable of driving strong outflows but also inducing star‐formation by pressure‐triggering collapse of dense clouds. We review theoretical work on negative and positive active galactic nuclei feedback, discussing insights gained from recent hydrodynamical simulations of jet‐driven feedback on galaxy scales that are applicable to compact radio sources. The simulations show that the efficiency of feedback and the relative importance of negative and positive feedback depend strongly on interstellar medium properties, especially the column depth and spatial distribution of clouds. Negative feedback is most effective if clouds are distributed spherically and in idual clouds have small column depths, while positive feedback is most effective if clouds are predominantly in a disc‐like configuration. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Cusp-to-core transition in low-mass dwarf galaxies induced by dynamical heating of cold dark matter by primordial black holes
Publisher: Oxford University Press (OUP)
Date: 28-01-2020
Abstract: We performed a series of high-resolution N-body simulations to examine whether dark matter candidates in the form of primordial black holes (PBHs) can solve the cusp–core problem in low-mass dwarf galaxies. If some fraction of the dark matter in low-mass dwarf galaxies consists of PBHs and the rest is cold dark matter, dynamical heating of the cold dark matter by the PBHs induces a cusp-to-core transition in the total dark matter profile. The mechanism works for PBHs in the 25–100 M⊙ mass window, consistent with the Laser Interferometer Gravitational-Wave Observatory (LIGO) detections, but requires a lower limit on the PBH mass fraction of 1 ${{\\rm per\\ cent}}$ of the total dwarf galaxy dark matter content. The cusp-to-core transition time-scale is between 1 and 8 Gyr. This time-scale is also a constant multiple of the relaxation time between cold dark matter particles and PBHs, which depends on the mass, the mass fraction, and the scale radius of the initial density profile of PBHs. We conclude that dark matter cores occur naturally in haloes composed of cold dark matter and PBHs, without the need to invoke baryonic processes.
Unravelling the enigmatic ISM conditions in Minkowski’s object
Publisher: Oxford University Press (OUP)
Date: 12-10-2020
Abstract: Local ex les of jet-induced star formation lend valuable insight into its significance in galaxy evolution and can provide important observational constraints for theoretical models of positive feedback. Using optical integral field spectroscopy, we present an analysis of the ISM conditions in Minkowski’s object (z = 0.0189), a peculiar star-forming dwarf galaxy located in the path of a radio jet from the galaxy NGC 541. Full spectral fitting with ppxf indicates that Minkowski’s object primarily consists of a young stellar population $\\sim \\! 10\\, \\rm Myr$ old, confirming that the bulk of the object’s stellar mass formed during a recent jet interaction. Minkowski’s object exhibits line ratios largely consistent with star formation, although there is evidence for a low level ($\\lesssim \\! 15 \\, \\rm per \\, cent$) of contamination from a non-stellar ionizing source. Strong-line diagnostics reveal a significant variation in the gas-phase metallicity within the object, with $\\log \\left(\\rm O / H \\right) + 12$ varying by $\\sim \\! 0.5\\, \\rm dex$, which cannot be explained by in-situ star formation, an enriched outflow from the jet, or enrichment of gas in the stellar bridge between NGC 541 and NGC 545/547. We hypothesize that Minkowski’s object either (i) was formed as a result of jet-induced star formation in pre-existing gas clumps in the stellar bridge, or (ii) is a gas-rich dwarf galaxy that is experiencing an elevation in its star formation rate due to a jet interaction, and will eventually redden and fade, becoming an ultradiffuse galaxy as it is processed by the cluster.
Ionized Gas Outflows in Infrared-bright Dust-obscured Galaxies Selected withWISEand SDSS
Publisher: American Astronomical Society
Date: 27-11-2017
Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We report the results of joint Chandra/ACIS—NuSTAR deep observations of NGC 1167, the host galaxy of the young radio jet B2 0258+35. In the ACIS data, we detect X-ray emission, extended both along and orthogonal to the jet. At the end of the southeast radio jet, we find lower-energy X-ray emission that coincides with a region of CO turbulence and fast outflow motions. This suggests that the hot interstellar medium (ISM) may be compressed by the jet and molecular outflow, resulting in more efficient cooling. Hydrodynamic simulations of jet–ISM interaction tailored to NGC 1167 are in agreement with this conclusion and with the overall morphology and spectra of the X-ray emission. The faint hard nuclear source detected with Chandra and the stringent NuSTAR upper limits on the harder X-ray emission show that the active galactic nucleus (AGN) in NGC 1167 is in a very low-accretion state. However, the characteristics of the extended X-ray emission are more consonant to those of luminous Compton-thick (CT) AGNs, suggesting that we may be observing the remnants of a past high accretion rate episode, with sustained strong activity lasting ∼2 × 10 3 yr. We conclude that NGC1167 is presently a Low-Ionization Nuclear Emission-line Region (LINER) , but was an AGN in the past, given the properties of the extended X-ray emission and their similarity with those of CT AGN extended emission.
Tracing the Milky Way’s Vestigial Nuclear Jet
Publisher: American Astronomical Society
Date: 12-2021
Abstract: MeerKAT radio continuum and XMM-Newton X-ray images have recently revealed a spectacular bipolar channel at the Galactic Center that spans several degrees (∼0.5 kpc). An intermittent jet likely formed this channel and is consistent with earlier evidence of a sustained, Seyfert-level outburst fueled by black hole accretion onto Sgr A* several Myr ago. Therefore, to trace a now weak jet that perhaps penetrated, deflected, and percolated along multiple paths through the interstellar medium, relevant interactions are identified and quantified in archival X-ray images, Hubble Space Telescope Paschen α images and Atacama Large Millimeter/submillimeter Array millimeter-wave spectra, and new SOAR telescope IR spectra. Hydrodynamical simulations are used to show how a nuclear jet can explain these structures and inflate the ROSAT/eROSITA X-ray and Fermi γ -ray bubbles that extend ± 75° from the Galactic plane. Thus, our Galactic outflow has features in common with energetic, jet-driven structures in the prototypical Seyfert galaxy NGC 1068.
Cold gas removal from the centre of a galaxy by a low-luminosity jet
Publisher: Springer Science and Business Media LLC
Date: 10-02-2022
AGN feedback by relativistic jets
Publisher: Cambridge University Press (CUP)
Date: 09-2015
DOI: 10.1017/S174392131500201X
Abstract: Feedback provided by relativistic jets may be effective in shaping the galaxy luminosity function. The quenching mode (quasar mode) at redshifts ~2-3 potentially disperses gas in star-forming galaxies. The maintenance mode (radio mode) heats the gas in galaxy clusters counteracting cooling flows. A number of authors have examined the effect of relativistic jets in dispersing clouds in the kpc-scale inhomogeneous interstellar medium of evolving galaxies. We have also investigated a particular case of maintenance-mode feedback in our simulation of the iconic radio galaxy / cooling flow cluster Hydra A. Modelling of the knots produced by the jets in the inner 10 kpc provides an estimate of 0.8 – 0.9 c for the velocities of the jets in agreement with other velocity estimates for FR1 jets. The addition of jet precession provides realistic simulations of the morphology of the Hydra A radio source and raises interesting questions as to the role of black hole and disk precession, in general, in galaxy formation.
Impact of relativistic jets on the star formation rate: a turbulence-regulated framework
Publisher: Oxford University Press (OUP)
Date: 02-10-2021
Abstract: We apply a turbulence-regulated model of star formation to calculate the star formation rate (SFR) of dense star-forming clouds in simulations of jet–interstellar medium (ISM) interactions. The method isolates in idual clumps and accounts for the impact of virial parameter and Mach number of the clumps on the star formation activity. This improves upon other estimates of the SFR in simulations of jet–ISM interactions, which are often solely based on local gas density, neglecting the impact of turbulence. We apply this framework to the results of a suite of jet–ISM interaction simulations to study how the jet regulates the SFR both globally and on the scale of in idual star-forming clouds. We find that the jet strongly affects the multiphase ISM in the galaxy, inducing turbulence and increasing the velocity dispersion within the clouds. This causes a global reduction in the SFR compared to a simulation without a jet. The shocks driven into clouds by the jet also compress the gas to higher densities, resulting in local enhancements of the SFR. However, the velocity dispersion in such clouds is also comparably high, which results in a lower SFR than would be observed in galaxies with similar gas mass surface densities and without powerful radio jets. We thus show that both local negative and positive jet feedback can occur in a single system during a single jet event, and that the SFR in the ISM varies in a complicated manner that depends on the strength of the jet–ISM coupling and the jet break-out time-scale.
Relativistic jet feedback - III. Feedback on gas discs
Publisher: Oxford University Press (OUP)
Date: 05-07-2018
The Formation and Physical Origin of Highly Ionized Cooling Gas
Publisher: American Astronomical Society
Date: 23-10-2017
AGN feedback compared: jets versus radiation
Publisher: Oxford University Press (OUP)
Date: 15-03-2018
DOI: 10.1093/MNRAS/STY708
Relativistic Jets in Active Galactic Nuclei
Publisher: Journal of the Physical Society of Japan
Date: 19-03-2014
Extreme gaseous outflows in radio-loud narrow-line Seyfert 1 galaxies
Publisher: Oxford University Press (OUP)
Date: 17-04-2018
DOI: 10.1093/MNRAS/STY901
Two-fluid models of cosmic-ray modified radiative shocks including the effects of an acoustic instability
Publisher: EDP Sciences
Date: 20-11-2006
Feedback from low-luminosity radio galaxies: B2 0258+35
Publisher: EDP Sciences
Date: 09-2019
DOI: 10.1051/0004-6361/201935931
Abstract: Low-luminosity radio-loud active galactic nuclei (AGN) are of importance in studies concerning feedback from radio AGN since a dominant fraction of AGN belong to this class. We report high-resolution Very Large Array (VLA) and European VLBI Network (EVN) observations of H I 21 cm absorption from a young, compact steep-spectrum radio source, B2 0258+35, nested in the early-type galaxy NGC 1167, which contains a 160 kpc H I disc. Our VLA and EVN H I absorption observations, modelling, and comparison with molecular gas data suggest that the cold gas in the centre of NGC 1167 is very turbulent (with a velocity dispersion of ∼90 km s −1 ) and that this turbulence is induced by the interaction of the jets with the interstellar medium (ISM). Furthermore, the ionised gas in the galaxy shows evidence of shock heating at a few kpc from the radio source. These findings support the results from numerical simulations of radio jets expanding into a clumpy gas disc, which predict that the radio jets in this case percolate through the gas disc and drive shocks into the ISM at distances much larger than their physical extent. These results expand the number of low-luminosity radio sources found to impact the surrounding medium, thereby highlighting the possible relevance of these AGN for feedback.
ERRATUM: “RELATIVISTIC JET FEEDBACK IN EVOLVING GALAXIES” (2011, ApJ, 728, 29)
Publisher: American Astronomical Society
Date: 17-08-2011
Two-fluid models of cosmic ray modified radiative shocks
Publisher: EDP Sciences
Date: 06-2006
Tracing the Ionization Structure of the Shocked Filaments of NGC 6240
Publisher: American Astronomical Society
Date: 12-2021
Abstract: We study the ionization and excitation structure of the interstellar medium in the late-stage gas-rich galaxy merger NGC 6240 using a suite of emission-line maps at ∼25 pc resolution from the Hubble Space Telescope, Keck/NIRC2 with Adaptive Optics, and the Atacama Large Millimeter/submillimeter Array (ALMA). NGC 6240 hosts a superwind driven by intense star formation and/or one or both of two active nuclei the outflows produce bubbles and filaments seen in shock tracers from warm molecular gas (H 2 2.12 μ m) to optical ionized gas ([O iii ], [N ii ], [S ii ], and [O i ]) and hot plasma (Fe XXV ). In the most distinct bubble, we see a clear shock front traced by high [O iii ]/H β and [O iii ]/[O i ]. Cool molecular gas (CO(2−1)) is only present near the base of the bubble, toward the nuclei launching the outflow. We interpret the lack of molecular gas outside the bubble to mean that the shock front is not responsible for dissociating molecular gas, and conclude that the molecular clouds are partly shielded and either entrained briefly in the outflow, or left undisturbed while the hot wind flows around them. Elsewhere in the galaxy, shock-excited H 2 extends at least ∼4 kpc from the nuclei, tracing molecular gas even warmer than that between the nuclei, where the two galaxies’ interstellar media are colliding. A ridgeline of high [O iii ]/H β emission along the eastern arm aligns with the southern nucleus’ stellar disk minor axis optical integral field spectroscopy from WiFeS suggests this highly ionized gas is centered at systemic velocity and likely photoionized by direct line of sight to the southern active galactic nucleus.
Related Organisations
University Of Leeds
Location: United Kingdom of Great Britain and Northern Ireland
Harvard-Smithsonian Center For Astrophysics
Location: United States of America
ANU Research School Of Astronomy And Astrophysics
Location: Australia
Related Funding Activities
The Key Role Of Black Holes In Galaxy Evolution
Start Date: 2014
End Date: 2016
Funder: Australian Research Council
View Funded ActivityInterstellar Turbulence By Supermassive Black-Hole Jets, Winds, And Radiation
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End Date: 2022
Funder: Japan Society for the Promotion of Science
View Funded ActivityDiscovery Projects - Grant ID: DP140103341
Start Date: 2014
End Date: 12-2017
Amount: $399,231.00
Funder: Australian Research Council
View Funded Activity