Jet-regulated cooling catastrophe

By Y. Dubois, J. Devriendt, A. Slyz, Romain Teyssier. 2010

133 citations recorded by the source corpus.

We present the first implementation of active galactic nuclei (AGN) feedback in the form of momentum-driven jets in an adaptive mesh refinement (AMR) cosmological resimulation of a galaxy cluster. The jets are powered by gas accretion on to supermassive black holes (SMBHs) which also grow by mergers. Throughout its formation, the cluster experiences different dynamical states: both a morphologically perturbed epoch at early times and a relaxed state at late times allowing us to study the different modes of black hole (BH) growth and associated AGN jet feedback. BHs accrete gas efficiently at high redshift (z > 2), significantly pre-heating proto-cluster haloes. Gas-rich mergers at high redshift also fuel strong, episodic jet activity, which transports gas from the proto-cluster core to its outer regions. At later times, while the cluster relaxes, the supply of cold gas on to the BHs is reduced leading to lower jet activity. Although the cluster is still heated by this activity as sound waves propagate from the core to the virial radius, the jets inefficiently redistribute gas outwards and a small cooling flow develops, along with low-pressure cavities similar to those detected in X-ray observations. Overall, our jet implementation of AGN feedback quenches star formation quite efficiently, reducing the stellar content of the central cluster galaxy by a factor of 3 compared to the no-AGN case. It also dramatically alters the shape of the gas density profile, bringing it in close agreement with the β model favoured by observations, producing quite an isothermal galaxy cluster for gigayears in the process. However, it still falls short in matching the lower than universal baryon fractions which seem to be commonplace in observed galaxy clusters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/be106fc4a517fdaef27e0054ec1ceb87a0ff2ef2

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Citations in the corpus

AGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxies (2013, methodology): “We recall here the main aspects of this modelling, and refer to Dubois et al. (2010, 2012) for the technical issues.”
Black hole evolution – I. Supernova-regulated black hole growth (2015, background): “…on the galaxy mass content, the circumgalactic gas properties and the halo mass distribution can E-mail: dubois@iap.fr be dramatic (Di Matteo, Springel & Hernquist 2005; Bower et al. 2006; Croton et al. 2006; Sijacki et al. 2007; Booth & Schaye 2009; Dubois et al. 2010, 2012; Teyssier et al. 2011).”
Mechanical AGN feedback: controlling the thermodynamical evolution of elliptical galaxies (2012, methodology): “(ii) Many studies – including ours (G11a,b) – use the Bondi (1952) theory to estimate the instantaneous mass accretion rate on to the BH (Springel, Di Matteo & Hernquist 2005; Cattaneo & Teyssier 2007; Sijacki et al. 2007; Puchwein, Sijacki & Springel 2008; Booth & Schaye 2009; Dubois et al. 2010).”
Dancing in the dark: galactic properties trace spin swings along the cosmic web (2014, background): “Moreover, for massive galaxies, the feedback from the central AGN switches off later accretion of circumgalactic gas (Dubois et al. 2010).”
The Horizon-AGN Simulation: Morphological Diversity of Galaxies ,Promoted by AGN Feedback (2016, background): “The late radio mode of AGN feedback is also mandatory to gently shock-heat the gas in order to prevent the gas to catastrophic cool (Dubois et al. 2010, 2011), which can be seen in the temperature ripples (left and right side of the central galaxy) of the bottom left panel of Fig.”
DRIVING OUTFLOWS WITH RELATIVISTIC JETS AND THE DEPENDENCE OF ACTIVE GALACTIC NUCLEUS FEEDBACK EFFICIENCY ON INTERSTELLAR MEDIUM INHOMOGENEITY (2012, methodology): “…include the Hydra A (Wise et al. 2007), Perseus A (Fabian et al. 2006), and M87 in the Virgo Cluster (Million et al. 2010), and the phenomenon is well reproduced in cluster-scale grid-based hydrodynamic simulations by Gaspari et al. (2012), Dubois et al. (2010, 2011), and Teyssier et al. (2011).”
Towards a realistic population of simulated galaxy groups and clusters (2013, background): “…been overcome in simulations which include feedback from supermassive black holes (e.g. Springel, Di Matteo & Hernquist 2005; Sijacki et al. 2007; Dubois et al. 2010; Fabjan et al. 2010; McCarthy et al. 2010, 2011; Short, Thomas & Young 2013), while feedback from star formation and supernovae…”
The cosmic evolution of massive black holes in the Horizon-AGN simulation (2016, background): “…on the other hand, the radio mode deposits the AGN feedback energy into a bipolar outflow with a jet velocity of 104 km s−1 into a cylinder with a cross-section of radius x and height 2 x following Omma et al. (2004) (more details about the jet implementation are given in Dubois et al. 2010).”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, methodology): “These diagrams suggest that the feedback from AGNs at high redshifts is essentially dominated by a quasar mode (χ > 10−2), whereas at low redshift a radio mode (χ ≤ 10−2) prevails within the core of massive structures (Dubois et al. 2010).”
The impact of angular momentum on black hole accretion rates in simulations of galaxy formation (2013, background): “More recently, some papers have focused on modelling both feedback modes, quasar and radio, either making use of two accretion modes (Sijacki et al. 2007; Vogelsberger et al. 2014) or different ways of implementing jet feedback (Dubois et al. 2010; Debuhr, Quataert & Ma 2011).”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, background): “…reality, AGN activity may drive small-scale turbulent motions around the core region of clusters (e.g. Heinz et al.2006; Scannapieco & Bruggen 2009; Dubois et al.2010, Morsony et al.2010; Vazza 2010), while the interplay of tan-gled magnetic ﬁeld and Cosmic Rays is expected to inject chaotic…”
Simulating galaxy formation with black hole driven thermal and kinetic feedback (2016, background): “…Brighenti & Mathews 2006; Brüggen et al. 2007; Cattaneo & Teyssier 2007; Sternberg et al. 2007; Sternberg & Soker 2009; Gaspari et al. 2011a,b, 2012; Li & Bryan 2014a,b; Li et al. 2015; Hillel & Soker 2016; Yang & Reynolds 2016a,b), or in cosmological simulations (Dubois et al. 2010, 2012, 2016).”