A deep Chandra observation of the Perseus cluster: shocks and ripples

By A. C. Fabian, Jeremy S. Sanders, Steven W. Allen, C. Crawford, K. Iwasawa, R. Johnstone, Robert Schmidt, G. Taylor. 2003

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We present preliminary results from a deep observation lasting almost 200 ks of the centre of the Perseus cluster of galaxies around NGC 1275. The X-ray surface brightness of the intracluster gas beyond the inner 20 kpc, which contains the inner radio bubbles, is very smooth apart from some low-amplitude quasi-periodic ripples. A clear density jump at a radius of 24 kpc to the north-east, about 10 kpc out from the bubble rim, appears to be due to a weak shock driven by the northern radio bubble. A similar front may exist around both inner bubbles but is masked elsewhere by rim emission from bright cooler gas. The continuous blowing of bubbles by the central radio source, leading to the propagation of weak shocks and viscously dissipating sound waves seen as the observed fronts and ripples, gives a rate of working which balances the radiative cooling within the inner 50 kpc of the cluster core.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b848e3268690543e0210733f355eb69d9544ad3c

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Citations in the corpus

INTRACLUSTER MEDIUM ENTROPY PROFILES FOR A CHANDRA ARCHIVAL SAMPLE OF GALAXY CLUSTERS (2009, background): “…longer in doubt as evidenced by the prevalence of ICM bubbles (e.g., Bı̂rzan et al. 2004; Dunn & Fabian 2008), the possible presence of sound waves (Fabian et al. 2003; Sanders & Fabian 2008), and large-scale shocks associated with AGN outbursts (Forman et al. 2005; McNamara et al. 2005; Nulsen…”
Buoyant radio lobes in a viscous intracluster medium (2004, methodology): “The most detailed X-ray investigation to date, based on a deep (200 ks) observation by Chandra/ACIS-S, has been presented by Fabian et al. (2003a).”
Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction (2009, background): “If this were indeed the case, it would imply that AGN heating is achieved via mechanisms such as weak shocks (e.g., Fabian et al. 2003), or buoyant bubbles (e.g., Churazov et al. 2001), rather than via catastrophic explosions.”
Investigating AGN heating in a sample of nearby clusters (2006, background): “The energy also needs to be transported out to a large radius, for example, the viscous dissipation of sound waves in the ICM as they travel out in the cluster (Fabian et al. 2003a, 2005).”
The dark nemesis of galaxy formation : why hot haloes trigger black hole growth and bring star formation to an end (2016, background): “Observational measurements of energetic outflows and radio jets from galaxy nuclei (eg., Harrison et al. 2012; Maiolino et al. 2012; Fabian et al. 2003) indeed suggest that black holes play an important role in galaxy formation, most likely by heating the surrounding gas corona, offsetting cooling…”
ON THE CLUSTER PHYSICS OF SUNYAEV–ZEL'DOVICH AND X-RAY SURVEYS. I. THE INFLUENCE OF FEEDBACK, NON-THERMAL PRESSURE, AND CLUSTER SHAPES ON Y–M SCALING RELATIONS (2011, background): “These effects can seen to be dramatic in X-ray observations (e.g., Fabian et al. 2003), since the emission is proportional to gas density squared.”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, background): “This is likely to result from interactions between the central radio sources and surrounding gas (e.g. Böhringer et al. 1993; Fabian et al. 2000, 2003a, 2005, 2006; Birzan et al. 2004; Dunn & Fabian 2004; Forman et al. 2005; Dunn, Fabian & Taylor 2005; Allen et 3 Note that the outermost pressure,…”
The relation between accretion rate and jet power in X-ray luminous elliptical galaxies (2006, background): “Some additional energy will also be transfered into sound waves (Churazov et al. 2002; Fabian et al. 2003, 2005, 2006; Forman et al. 2003; Ruszkowski et al. 2004).”
The many lives of active galactic nuclei: cooling flows, black holes and the luminosities and colour (2005, background): “Tabor & Binney (1993) suggested that radio galaxies might regulate cooling flows, and this idea has gained considerable recent support from X-ray maps which show direct evidence for an interaction between radio lobes and the intracluster gas (McNamara et al. 2000, 2005; Fabian et al. 2003).”
RELATIVISTIC JET FEEDBACK IN EVOLVING GALAXIES (2010, background): “Their feedback prescription is motivated by the well-documented evidence for the effect of radio galaxies on “cooling flow” galaxies (Fabian et al. 2003; McNamara et al. 2005).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “This process is observed in the form of weak shocks or sound waves surrounding some radio bubbles, with the most striking example being the Perseus cluster where several concentric ripples in X-ray pressure are seen (Fabian et al. 2003, 2006).”
Properties of galaxy groups in the Sloan Digital Sky Survey – II. Active galactic nucleus feedback and star formation truncation (2006, background): “This has largely been motivated by X-ray observations which reveal that AGN can indeed impact the hot intergalactic medium (IGM) of galaxy clusters (e.g. Fabian et al. 2003; McNamara et al. 2005).”
AGN heating and ICM cooling in the HIFLUGCS sample of galaxy clusters (2008, background): “The AGN-blown cavities transfer heat to the ICM potentially by generating sound and weak shock waves (Jones et al. 2002; Fabian et al. 2003; Mathews et al. 2006), by doing pdV work against the ambient medium and dissipation of cavity enthalpy in the wake of buoyantly rising cavities (e.g.…”
Reflections of Active Galactic Nucleus Outbursts in the Gaseous Atmosphere of M87 (2003, background): “The gas temperature map was calculated as described by Churazov et al. (1996; see also Churazov et al. 2003 for this method applied to XMM-Newton data for the Perseus Cluster).”
AGN Feedback and Cooling Flows: Problems with Simple Hydrodynamic Models (2005, background): “In several clusters observed with Chandra, the ghost cavities are not symmetric about the cluster center (e.g., A4059, Heinz et al. (2002); Perseus-A, Fabian et al. (2003)), suggesting that they are buoyantly rising in an ICM atmosphere which itself has velocity structure.”
THE FUNDAMENTAL PLANE OF ACCRETION ONTO BLACK HOLES WITH DYNAMICAL MASSES (2009, background): “The impact of relativistic jets on the interstellar medium (Gallo et al. 2005b), and large-scale structure in clusters of galaxies (Allen et al. 2006; Fabian et al. 2003; McNamara et al. 2006), has become dramatically clear in the era of imaging and spectroscopy withChandra.”
Jet-regulated cooling catastrophe (2010, background): “These sound waves, provided one can dissipate them viscously (Fabian et al. 2003; Ruszkowski, Brüggen & Begelman 2004a), can reheat the ICM at distances larger than the scalelength of the jet.”