Relativistic jet feedback – III. Feedback on gas discs

Mukherjee, Dipanjan; Bicknell, G. V.; Wagner, Alexander Y.; Sutherland, Ralph S.; Silk, Joseph

doi:10.1093/mnras/sty1776

Cited by 200 publications

(288 citation statements)

References 129 publications

Supporting

Mentioning

258

Contrasting

Order By: Relevance

“…Recent numerical simulations (e.g. Cielo et al 2018;Mukherjee et al 2018a) also support the importance of this mode of feedback from radio AGN. They predict that jets expanding into a clumpy gas disc affect the gas kinematics significantly.…”

Section: Introductionmentioning

confidence: 80%

Feedback from low-luminosity radio galaxies: B2 0258+35

Murthy

Morganti

Oosterloo

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

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 21cm 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.

show abstract

Section: Introductionmentioning

confidence: 80%

Feedback from low-luminosity radio galaxies: B2 0258+35

Murthy

Morganti

Oosterloo

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Cutting-edge models show that compact jets interacting with the interstellar medium may be a crucial aspect of 'AGN feedback' and possibly the most efficient mechanism for driving powerful outflows (e.g., Wagner et al 2012;Mukherjee et al 2016;Bicknell et al 2018;Cielo et al 2018). For example, Mukherjee et al (2018) show that jets can increase the turbulence of the gas within the disc and simultaneously drive larger-scale outflowing bubbles, in qualitative agreement with the observations presented here for some of our targets (e.g., J1000+1242; J1356+1026; J1430+1339; see Fig. 10 and 11).…”

Section: Radio Jets Associated With Quasar Outflows and Feedbackmentioning

confidence: 99%

“…10 and 11). In future work, we will use our IFS data and radio imaging to measure the detailed outflow energetics in relation to the jet power and assess if the jets have a negative or positive impact on the star formation in their host galaxies (e.g., Mukherjee et al 2018).…”

Section: Radio Jets Associated With Quasar Outflows and Feedbackmentioning

confidence: 99%

Prevalence of radio jets associated with galactic outflows and feedback from quasars

Jarvis

Harrison

Thomson

et al. 2019

Monthly Notices of the Royal Astronomical Society

157

313

View full text Add to dashboard Cite

We present 1-7 GHz high-resolution radio imaging (VLA and e-MERLIN) and spatially-resolved ionized gas kinematics for ten z < 0.2 type 2 'obscured' quasars (log[L AGN /erg s −1 ] 45) with moderate radio luminosities (log[L 1.4 GHz /W Hz −1 ]=23.3-24.4). These targets were selected to have known ionized outflows based on broad [O iii] emission-line components (FWHM≈800-1800 km s −1 ). Although 'radio-quiet' and not 'radio AGN' by many traditional criteria, we show that for nine of the targets, star formation likely accounts for 10 per cent of the radio emission. We find that ∼80-90 per cent of these nine targets exhibit extended radio structures on 1-25 kpc scales. The quasars' radio morphologies, spectral indices and position on the radio size-luminosity relationship reveals that these sources are consistent with being low power compact radio galaxies. Therefore, we favour radio jets as dominating the radio emission in the majority of these quasars. The radio jets we observe are associated with morphologically and kinematically distinct features in the ionized gas, such as increased turbulence and outflowing bubbles, revealing jetgas interaction on galactic scales. Importantly, such conclusions could not have been drawn from current low-resolution radio surveys such as FIRST. Our observations support a scenario where compact radio jets, with modest radio luminosities, are a crucial feedback mechanism for massive galaxies during a quasar phase.

show abstract

“…average values of 0.01-0.1 reported in literature (Mukherjee et al 2018;Federrath & Klessen 2012. For the higher mass models, the efficiency parameter falls within the expected range, though the slope is not consistent with the KS relation.…”

Section: Star Formation Ratesmentioning

confidence: 89%

Gas inflow and star formation near supermassive black holes: the role of nuclear activity

Frazer

Heitsch

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Numerical models of gas inflow towards a supermassive black hole (SMBH) show that star formation may occur in such an environment through the growth of a gravitationally unstable gas disc. We consider the effect of nuclear activity on such a scenario. We present the first three-dimensional grid-based radiative hydrodynamic simulations of direct collisions between infalling gas streams and a 4 × 10 6 M SMBH, using raytracing to incorporate radiation consistent with an active galactic nucleus (AGN). We assume inflow masses of ≈ 10 5 M and explore radiation fields of 10% and 100% of the Eddington luminosity (L edd ). We follow our models to the point of central gas disc formation preceding star formation and use the Toomre Q parameter (Q T ) to test for gravitational instability. We find that radiation pressure from UV photons inhibits inflow. Yet, for weak radiation fields, a central disc forms on timescales similar to that of models without feedback. Average densities of > 10 8 cm −3 limit photo-heating to the disc surface allowing for Q T ≈ 1. For strong radiation fields, the disc forms more gradually resulting in lower surface densities and larger Q T values. Mass accretion rates in our models are consistent with 1%-60% of the Eddington limit, thus we conclude that it is unlikely that radiative feedback from AGN activity would inhibit circumnuclear star formation arising from a massive inflow event.

show abstract

Relativistic jet feedback – III. Feedback on gas discs

Cited by 200 publications

References 129 publications

Feedback from low-luminosity radio galaxies: B2 0258+35

Feedback from low-luminosity radio galaxies: B2 0258+35

Prevalence of radio jets associated with galactic outflows and feedback from quasars

Gas inflow and star formation near supermassive black holes: the role of nuclear activity

Contact Info

Product

Resources

About