Hydrodynamical simulations of cluster formation with central AGN heating

By D. Sijacki, V. S. I. O. T. Astrophysics, Garching, Heidelberg · Germany. 2005

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We analyse the effects of central AGN heating on the formation of galaxy clusters by means of hydrodynamical simulations. Besides self-gravity of dark matter and baryons, our approach includes radiative cooling and heating processes of the gas component and a multiphase model for a self-consistent treatment of star formation and SNe feedback [1]. Additionally, we incorporate a periodic feedback mechanism in the form of hot buoyant bubbles, injected into the ICM during the active phases of accreting central AGN. We find that AGN heating can substantially affect the properties of the stellar and gaseous components, in particular reducing the mass deposition rate onto the central cD galaxy, thereby offering an energetically plausible solution to the cooling flow problem.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/71ba8a5ba76118f82d11c05b7edefbb20da5946e

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Citations in the corpus

Chemical enrichment of galaxy clusters from hydrodynamical simulations (2007, methodology): “While approaches to include physical viscosity in the SPH scheme have been recently pursued (Sijacki & Springel 2006b), a full accounting for its effect requires including a self-consistent description of the magnetic field which suppresses the mean-free path of ions.”
AGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxies (2013, background): “…also confirm that this mechanism is able to self-regulate the baryon content in massive haloes to get realistic galaxy masses and colours (Sijacki & Springel 2006; Puchwein, Sijacki & Springel 2008; Khalatyan et al. 2008; McCarthy et al. 2010, 2011; Dubois et al. 2010, 2011; Teyssier et…”
A deeper X‐ray study of the core of the Perseus galaxy cluster: the power of sound waves and the distribution of metals and cosmic rays (2007, background): “Ripples due to sound waves have since been found in simulations (Ruszkowski, Brüggen & Begelman 2004; Sijacki & Springel 2006).”
Cosmic ray feedback in hydrodynamical simulations of galaxy formation (2006, background): “In most current models of galaxy formation, feedback effects due to supernovae explosions and due to a photoionizing background are usually included, and more recently, some studies have considered quasar and radio activity by AGN as well (e.g. Di Matteo et al., 2005; Sijacki & Springel, 2006).”
A model for cosmological simulations of galaxy formation physics: multi-epoch validation (2013, background): “…et al. 2013), and more recently also AGN feedback (e.g., Springel et al. 2005b; Kawata & Gibson 2005; Di Matteo et al. 2005; Thacker et al. 2006; Sijacki & Springel 2006; Sijacki et al. 2007; Di Matteo et al. 2008; Okamoto et al. 2008; Booth & Schaye 2009; Kurosawa & Proga 2009; Teyssier et…”
Simulating the effect of active galactic nuclei feedback on the metal enrichment of galaxy clusters (2009, methodology): “This model has been modified by Sijacki & Springel (2006) who included the possibility to inflate high-entropy bubbles in the ICM whenever accretion onto the central BH enters in a quiescent “radio mode”.”
Gravitational quenching in massive galaxies and clusters by clumpy accretion (2007, background): “This is as long as they do not incorporate another heating source such as AGN feedback that is practically put by hand (e.g. Sijacki & Springel 2006, and references therein).”
Galaxies in a simulated ΛCDM universe – II. Observable properties and constraints on feedback (2009, background): “…model requires that most galaxies do not return to a star-forming phase after the star formation initially stops, so a long-term preventive feedback mechanism is still necessary to prevent further gas accretion, perhaps ‘radio mode’ AGN feedback (Ciotti & Ostriker 2001; Sijacki & Springel 2006).”
Breaking the hierarchy of galaxy formation (2005, background): “…idea that has gained popularity in recent years is that energy injected from AGN in the form of radio jets is responsible for switching off cooling at the centre of massive haloes (Quilis et al. 2001; Bruggen & Kaiser 2002; Churazov et al. 2002; Dalla Vecchia et al. 2004; Sijacki & Springel 2006).”
The case for AGN feedback in galaxy groups (2009, methodology): “Using the model of SDH05 as a backbone, Sijacki & Springel (2006), Sijacki et al. (2007), Puchwein et al. (2008), Bhattacharya et al. (2009), and Fabjan et al. (2009) examined the effects of AGN feedback1 on groups and clusters.”
Radiative efficiency, variability and Bondi accretion on to massive black holes: the transition from radio AGN to quasars in brightest cluster galaxies (2012, background): “Springel, Di Matteo & Hernquist 2005; Croton et al. 2006; Sijacki & Springel 2006; Hopkins et al. 2006; Bower et al. 2006).”
Measuring the kinetic power of active galactic nuclei in the radio mode (2007, background): “…flow riddle (see e.g. Fabian et al. 2001 and reference therein) in clusters of galaxies has been put forward by many in recent years (Binney & Tabor 1995; Begelman 2001; Churazov et al. 2001; Churazov et al. 2002; Dalla Vecchia et al. 2004; Sijacki & Springel 2006; Cattaneo & Teyssier 2007).”
Properties of galaxy groups in the Sloan Digital Sky Survey – II. Active galactic nucleus feedback and star formation truncation (2006, background): “On the other hand, Croton et al. (2006), Bower et al. (2006), Cattaneo et al. (2006a), Nusser, Silk & Babul (2006) and Sijacki & Springel (2006) have argued that the ‘radio mode’ of AGN activity (or AGN feedback operating in quasi-hydrostatically cooling haloes) is the main mechanism to truncate…”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, background): “…& Hernquist 2003a; Oppenheimer & Davé 2006; Hopkins, Quataert & Murray 2011), black hole growth and feedback (Springel, Di Matteo & Hernquist 2005a; Sijacki & Springel 2006; Booth & Schaye 2009; Dubois et al. 2012), magnetic fields (Dolag 2006; Pakmor, Marinacci & Springel 2014), and cosmic rays…”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, methodology): “In both the Croton et al. (2006) and Sijacki & Springel (2006) models, the correlation between black hole mass and bulge mass is imprinted during the quasar era and changes little at late times, when the suppression of cooling flows becomes important.”
A unified model for AGN feedback in cosmological simulations of structure formation (2007, methodology): “The initial gas density profile has a similar form as the dark matter, but with a slightly softened core, as explained in more detail in Sijacki & Springel (2006).”