The Properties of the X-Ray Holes in the Intracluster Medium of the Perseus Cluster

By A. C. Fabian, A. Celotti, K. Blundell, N. Kassim, R. Perley. 2001

158 citations recorded by the source corpus.

Abstract : High-resolution X-ray and low-frequency radio imaging now allow us to examine in detail the interaction and physical properties of the radio source 3C 84 and the surrounding thermal gas. The radiative and dynamical properties of the inner X-ray holes, which coincide with the radio lobes, indicate that the ratio of the energy factor k to the filling factor f is in the range 180 < k/f < 500. We define k to be the ratio of the total particle energy to that of the electrons radiating above a fiducial frequency of 10 MHz. The relativistic plasma and magnetic field are not in equipartition, since the field must be a factor of 4 or more lower than required for pressure balance. Unexpected steep-spectrum spurs in the low-frequency radio maps point to outer X-ray holes, which are plausibly buoyant old radio lobes. The evidence that the inner lobes are currently expanding subsonically, yet have not detached due to buoyancy, and the requirement that the synchrotron cooling time must exceed the age of the hole enable us to constrain the jet power of the nucleus to between 10(exp 44) and 10(exp 45) erg s (exp-1), depending on the filling factor of the relativistic plasma.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9bce66214213728bf6d3281335966c8ca0e5caeb

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

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, methodology): “…compilation C© 2007 RAS Downloaded from https://academic.oup.com/mnras/article-abstract/381/4/1381/971565 by guest on 28 July 2018 field (Churazov et al. 2000; Fabian et al. 2000), an idea supported by weak low-frequency radio spurs seen pointing towards their direction (Fabian et al. 2002b).”
The relationship between the optical Hα filaments and the X‐ray emission in the core of the Perseus cluster (2003, background): “This yields a lower limit on the viscosity of the intracluster medium of ν = uL/1000 orν > 4× 1027 cm2 s−1 assuming 700 km s−1 for u (Fabian et al 2002) and 20 kpc forL.”
Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster (2002, background): “Although it contains a wide-angle tail (WAT) radio source, there are no coincident X-ray ‘‘ holes,’’ such as those found in the clusters Hydra A (Nulsen et al. 2002) and Perseus (Fabian et al. 2002).”
Buoyant radio lobes in a viscous intracluster medium (2004, background): “This has led several authors (Narayan & Medvedev 2001; Fabian et al. 2002b; Voigt et al. 2002; Kim & Narayan 2003) to resurrect the notion that thermal conduction may be important in determining the thermodynamics of ICM cores.”
A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction (2005, methodology): “…acf@ast.cam.ac.uk We have previously observed the Perseus cluster with the Chandra Observatory for 25 ks (Fabian et al 2000; Schmidt et al 2002; Fabian et al 2002), 200 ks (Fabian et al 2003a,b, Sanders et al 2004, 2005) and now present here the first results from a further 800 ks of…”
A deep Chandra observation of the Perseus cluster: shocks and ripples (2003, background): “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.”
Hot Gas In and Around Elliptical Galaxies (2003, background): “Nonradiating relativistic protons may also be present (e.g. Fabian et al. 2002a), so it is unclear if Pnt can always be ignored.”
Jet-regulated cooling catastrophe (2010, background): “Observational evidence for strong AGN activity in groups and clusters is plenty (Arnaud et al. 1984; Carilli, Perley & Harris 1994; McNamara et al. 2001, 2005; Fabian et al. 2002; Bı̂rzan et al. 2004; Forman et al. 2007).”
Measuring the kinetic power of active galactic nuclei in the radio mode (2007, methodology): “…estimates of the jet power are also available based on detailed modelling of either radio emission in the jets and lobes (Cyg A, Carilli & Barthel 1996; M87, Bicknell & Begelman 1996; Per A, Fabian et al. 2002), or shock in the IGM induced by the expanding cocoons (NGC 4636, Jones et al. 2007).”
Cold molecular gas in cooling flow clusters of galaxies (2003, background): “Chandra images from Fabian et al. (2002) or Johnstone et al. (2002) have pointed out holes coincident with radio lobes and cold fronts showing the interaction between the radio source and the intra-cluster medium (e.g. in Hydra A, the Perseus cluster, Abell 1795, Abell 2199, the Virgo cluster).”
Cluster Heating by Viscous Dissipation of Sound Waves (2003, background): “…observations suggest that the actual inflow rates are much smaller than expected, and that feedback from active galactic nuclei (AGN) may play a crucial role in regulating mass accretion rates (e.g., Fabian et al. (2000, 2002); McNamara et al. (2000); Blanton et al. (2001); Churazov et al. (2002)).”
Reflections of Active Galactic Nucleus Outbursts in the Gaseous Atmosphere of M87 (2003, background): “Rims of cool gas are a common feature of cavities created by radio lobes (e.g., Finoguenov & Jones 2001; McNamara et al. 2000; Fabian et al. 2002; Blanton et al. 2001).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “Several studies have shown that at equipartition, lobe pressures are approximately an order of magnitude smaller than the surrounding gas pressure (Blanton et al. 2001; Fabian et al. 2002; De Young 2006).”
X-ray Spectroscopy of Cooling Clusters (2005, background): “…examining numerical simulations and then the heating mechanism in detail, we note that the total energy required to stave of cooling for several Gyr in a luminous cluster implies a large central black hole mass (Fabian et al. 2002; assuming a mass-to-energy conversion effiency of 10 per cent).”
XMM-Newton Observations of the Perseus Cluster. I. The Temperature and Surface Brightness Structure (2003, background): “…probably dominated by the interaction of the thermal gas with the central AGN radio lobes (e.g., Böhringer et al., 1993; Churazov et al. 2000; Fabian et al. 2000, 2002) there are two regions of prominent excess emission on large scale—one 40–70 west of the center and one 50 east of the…”