Observational Evidence of Active Galactic Nuclei Feedback

By A. C. Fabian. 2012

1,408 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/87c6ad216296ec2f374dbe77bfdc91b499105505

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Citations in the corpus

Theoretical Challenges in Galaxy Formation (2016, background): “Jets from AGN are frequently observed and feedback from this mechanism is sometimes Theoretical Challenges in Galaxy Formation 39 called ’radio mode’ (Fabian 2012, Heckman & Best 2014).”
Compaction and quenching of high-z galaxies in cosmological simulations: blue and red nuggets (2014, neutral): “…virial shock heating (Birnboim & Dekel 2003; Kereš et al. 2005; Dekel & Birnboim 2006; Kereš et al. 2009), by gravitational infall heating (Dekel & Birnboim 2008; Khochfar & Ostriker 2008), or by AGN feedback coupled to the hot halo gas (Dekel & Birnboim 2006; Cattaneo et al. 2009; Fabian 2012).”
AGN wind scaling relations and the co-evolution of black holes and galaxies (2017, methodology): “The power to excavate cavities in the ICM is proportional to the X-ray luminosity, and the power in cavities is proportional to the AGN radio luminosity (see McNamara & Nulsen 2007; Cattaneo et al. 2009; Fabian 2012, for reviews).”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, background): “In addition, highly relativistic giant radio jets may heat the intra-cluster medium through bubbles, weak shocks, and sound waves (Fabian 2012, McNamara & Nulsen 2007).”
Cool Gas in High-Redshift Galaxies (2013, background): “…galaxies at intermediate redshift (e.g., Feruglio et al. 2010), while powerful radio jets from AGN may be needed to heat the intercluster gas around massive galaxies at late cosmic epochs, thereby inhibiting further late–time growth of massive galaxies (Fabian 2012; McNamara & Nulsen 2007).”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, background): “Also, using a non-relativistic code and flux-limited diffusion, super-Eddington accretion flows have been simulated and their spectra computed (Ohsuga et al. 2003; Ohsuga et al. 2005; Ohsuga 2006; Ohsuga et al. 2009; Ohsuga & Mineshige 2011; Kawashima et al. 2012; Mineshige et al. 2012; Takeuchi et ”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, background): “On the other hand, AGN feedback is widely believed to play a crucial role in galaxy formation and evolution (Fabian 2012; Kormendy & Ho 2013), while winds produced by the AGN accretion flow is one of the most important ingredients for such a feedback because they could interact with the ISM in the…”
Hot Accretion Flows Around Black Holes (2014, background): “Bubbles and cavities in X-ray and radio images (e.g., Fabian 2012, Morganti et al. 2013) provide direct observational evidence for interaction between jets and the interstellar or intracluster medium.”
A remarkably flat relationship between the average star formation rate and AGN luminosity for distant X-ray AGN. (2015, background): “However, the scales of AGN activity and star formation are very different, which has lead to suggestions that any tight connection between them must be due to one process regulating the other (see Alexander & Hickox 2012; Fabian 2012; Kormendy & Ho 2013 for recent reviews).”
Ionised outflows in z $\sim$ 2.4 quasar host galaxies (2015, background): “Essentially, the observed correlations can be explained as the result of the balance between the outward radiation force generated by the AGN and the inward gravitional force of the host galaxy (e.g. King 2010; Fabian 2012).”
Diffuse Radio Emission from Galaxy Clusters (2019, background): “In the absence of a heating source, a cooling flow is expected to develop, whereby the tem- perature in the central region of the cluster drops and gas flows inwards (e.g., Fabian 1994; Peterson & Fabian 2006; Fabian 2012; McNamara & Nulsen 2012).”
MOJAVE. XV. VLBA 15 GHz Total Intensity and Polarization Maps of 437 Parsec-scale AGN Jets from 1996 to 2017 (2017, background): “…from powerful active galactic nuclei (AGNs) represent some of the most long-lived and energetic processes ever discovered, and are now recognized to have played a prominent role in the early structure formation of our universe via feedback mechanisms (e.g., Fabian 2012; Heckman & Best 2014).”
HIGH-RESOLUTION LINEAR POLARIMETRIC IMAGING FOR THE EVENT HORIZON TELESCOPE (2016, background): “In active galactic nuclei (AGNs), magnetic fields in accretion disks around central supermassive black holes regulate outflow and the interaction of the AGN with its host galaxy (Fabian 2012; Kormendy & Ho 2013).”
Galaxy Interactions Trigger Rapid Black Hole Growth: an unprecedented view from the Hyper Suprime-Cam Survey (2017, background): “…or cluster environments, evidence of AGN feedback due to radio emission from the BH present in the brightest cluster galaxy (so called, maintenance mode feedback) has long been established (e.g., Best et al. 2005; Rafferty et al. 2006; McNamara & Nulsen 2007; Kauffmann et al. 2008; Fabian 2012).”
Gravitational torque-driven black hole growth and feedback in cosmological simulations (2016, background): “Recent years have seen increasing observational evidence for AGN feedback, from radioemitting jets powered by slowly accreting black holes to powerful winds driven by quasars (Fabian 2012; Heckman & Best 2014).”
Black hole evolution – I. Supernova-regulated black hole growth (2015, background): “The energetics involved in growing BHs are in principle comparable to, C© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society if not higher than, the binding energy of the host galaxy (e.g. Silk & Rees 1998; Fabian 2012).”
Radio galaxies and feedback from AGN jets (2020, background): “portion of the z > 1 HERG population are likely to be ‘over-heating’ their environments: this population could be responsible for the known excess entropy present in hot gas haloes at low mass (e.g., Pratt et al., 2009; Short et al., 2010; Fabian, 2012).”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS (2012, background): “One important reason is because it is believed that AGNs feedback plays an important role in galaxy formation and evolution (e.g., Di Matteo et al. 2005; Hopkins et al. 2005; Fabian 2012).”