Chandra imaging of the complex X-ray core of the Perseus cluster

By A. C. Fabian, Jeremy S. Sanders, S. Ettori, G. Taylor, S. Allen, C. Crawford, K. Iwasawa, R. Johnstone, Patrick Ogle. 2000

472 citations recorded by the source corpus.

ABSTRACT We report subarcsec-resolution X-ray imaging of the core ofthe Perseus cluster around thegalaxy NGC1275 with the Chandra X-ray Observatory. The ROSAT-discovered holes asso-ciated with the radio lobes have X-ray bright rims which are cooler than the surrounding gasand not due to shocks. The holes themselves may contain some hotter gas. We map strongphotoelectric absorption across the Northern lobe and rim due to a small infalling irregulargalaxy, known as the high velocity system. Two outer holes, one of which was previouslyknown, are identiﬁed with recently found spurs of low-frequency radio emission. The spiralappearance of the X-ray cooler gas and the outer optical parts of NGC1275 may be due toangular momentum in the cooling ﬂow.Key words: galaxies: individual: Perseus – cooling ﬂows – galaxies: in dividual: NGC1275– X-rays: galaxies 1 INTRODUCTIONThe Perseus cluster, Abell426, at a redshift z = 0.0183 or dis-tance about 100 Mpc is the brightest cluster in the sky in X-rays. Ithosts the nearest large cooling ﬂow (e.g. Fabian et al 1981; A llenet al 1990; Fabian et al 1994). X-ray analysis of ASCA spectrain-dicates that the mass deposition rate is about 300M

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The Cluster-Scale AGN Outburst in Hydra A (2004, background): “…fed by AGN have created cavities in the hot gas in a growing number of clusters (Böhringer et al. 1993; Carilli et al. 1994; McNamara et al. 2000; Fabian et al. 2000; McNamara et al. 2001; Blanton et al. 2001; Schindler et al. 2001; Heinz et al. 1 Harvard-Smithsonian Center for Astrophysics, 60…”
Evolution of Buoyant Bubbles in M87 (2000, background): “New Chandra and XMM observations of cooling ﬂow clusters (e.g. McNamara et al. 2000, Fabian et al. 2000a) demonstrate that the interaction of the radio sources and thermal gas is widespread in these objects.”
Measuring the kinetic power of active galactic nuclei in the radio mode (2007, background): “…Ferrarese & Merritt 2000; Marconi & Hunt 2003), as well as into the disturbed morphology of the hot, X-ray emitting atmospheres of groups and clusters harboring active SMBH in their centers (Böhringer et al. 1993; Fabian et al. 2000; Churazov et al. 2002; Bı̂rzan et al. 2004; Fabian et al. 2006).”
The relation between accretion rate and jet power in X-ray luminous elliptical galaxies (2006, background): “…have shown that the black holes at the centres of galaxies, groups and clusters interact strongly with their environments, blowing clear cavities or ‘bubbles’ in the surrounding X-ray emitting gas (e.g. Böhringer et al. 1993; Fabian et al. 2000, 2003, 2005; Birzan et al. 2004; Forman et al. 2005).”
Hydrodynamical simulations of cluster formation with central AGN heating (2005, background): “In the past few years, a growing number of observations performed with the Chandra X-ray telescope have found the presence of so-called X-ray cavities in central galaxy cluster regions (e.g. McNamara et al. 2000; Fabian et al. 2000; Sanders & Fabian 2002; Mazzotta et al. 2002; Bîrzan et al. 2004).”
Supermassive black holes in elliptical galaxies: switching from very bright to very dim (2005, background): “These outflows usually manifest themselves as bubbles of radio emitting plasma coincident with depressions in the X-ray images (e.g. Böhringer et al. 1993; Fabian et al. 2000; McNamara et al. 2000).”
Hot Gas In and Around Elliptical Galaxies (2003, background): “In other cases, the radio-X-ray connection is less clear: Perseus/NGC 1275 (Böhringer et al. 1993; Fabian et al 2000; Churazov et al. 2000), A2052 (Blanton et al. 2001b) or A4059 (Heinz et al. 2002).”
On the soft X-ray spectrum of cooling flows (2000, background): “Observations of cooling flows around radio sources, e.g. 3C 295 (Allen et al. 2001b) and 3C 84 (Fabian et al. 2000), show no evidence for heating taking place beyond the radio lobes, which occupy only a small fraction of the volume.”
Adaptive binning of X‐ray data with weighted Voronoi tessellations (2005, methodology): “The smooth colour gradient toward the centre also supports a cooling flow model (see e.g. Sarazin 1988) and the “swirl” of the bright emission has been interpreted as a sign for angular momentum of the infalling gas (Fabian et al. 2000).”
Broad emission lines for a negatively spinning black hole (2010, background): “Observations of cavities in nearby galaxy clusters are also evidence for spin evolution (Wise et al. 2007; Fabian et al. 2000).”
On the prevalence of radio‐loud active galactic nuclei in brightest cluster galaxies: implications for AGN heating of cooling flows (2006, background): “…in recent years, as X-ray observations have revealed bubbles and cavities in the hot intracluster medium of some clusters, coincident with the lobes of the radio sources (e.g. Böhringer et al. 1993; Carilli, Perley & Harris 1994; Fabian et al. 2000; McNamara et al. 2000; Blanton et al. 2001).”
Chandra observations of Abell 2199 (2002, background): “For the case of the eastern radio lobe it may be that the radio-emitting plasma displaces the hot gas as is seen in the Perseus (Fabian et al. 2000) and other clusters (e.g. McNamara et al. 2000).”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, methodology): “The bubbles, discussed by Böhringer et al. (1993), Churazov et al. (2000) and Fabian et al. (2000, 2002a), are inflated by the north–south radio jets from the nucleus of NGC 1275.”
Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “However, although X-ray cavities are common in cooling core clusters (e.g., Fabian et al. 2000; McNamara et al. 2000; Blanton et al. 2001; Heinz et al. 2002; Mazzotta et al. 2003), the associated thermal gas and radio emission characteristic of a large buoyant bubble (Owen et al. 2000; Churazov et…”
XMM—Newton observations of the Perseus cluster — II. Evidence for gas motions in the core (2003, background): “Judging from the size of the observed radio lobes in the Perseus cluster (Böhringer et al. 1993, Fabian et al. 2000) one can expect the size of the generated eddies to be of order 10 kpc, i.e. sufficiently small to dissipate their energy quickly (compared to the timescale for radiative cooling).”