Radio bubbles in clusters of galaxies

By R. Dunn, A. C. Fabian, G. I. F. Astronomy, Cambridge, Nrao, Socorro, K. Institute, California. 2005

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We extend our earlier work on cluster cores with distinct radio bubbles, adding more active bubbles, i.e. those with GHz radio emission, to our sample, and also investigating “ghost bubbles,” i.e. those without GHz radio emission. We have determined k, which is the ratio of the total particle energy to that of the electrons radiati ng between 10 MHz and 10 GHz. Constraints on the ages of the active bubbles confirm that the ratio of the energy factor, k, to the volume filling factor, f lies within the range 1 . k/f . 1000. In the assumption that there is pressure equilibrium between the radio-emitting plasma and the surrounding thermal X-ray gas, none of the radio lobes has equipartition between the relativistic particles and the magnetic field. A Monte-Carlo simulation of the data led t o the conclusion that there are not enough bubbles present in the current sample to be able to determine the shape of the population. An analysis of the ghost bubbles in our sample showed that on the whole they have higher upper limits on k/f than the active bubbles, especially when compared to those in the same cluster. A study of the Brightest 55 cluster sample shows that 17, possibly 20, clusters required some form of heating as they have a short central cooling time, tcool 6 3 Gyr, and a large central temperature drop, Tcentre/Touter < 1/2. Of these between 12 (70 per cent) and 15 (75 per cent), contain bubbles. This indicates that the du ty cycle of bubbles is large in such clusters and that they can play a major role in the heating process.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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Citations in the corpus

Radio galaxies and feedback from AGN jets (2020, background): “, 1998) and subsequently found in many clusters and studied in depth using Chandra (e.g., Dunn and Fabian, 2004; Dunn et al., 2005; Bı̂rzan et al., 2004; Bı̂rzan et al., 2008).”
A RELATIONSHIP BETWEEN AGN JET POWER AND RADIO POWER (2010, background): “Studies of X-ray cavities have shown that AGN feedback supplies enough energy to regulate star formation and suppress cooling of the hot halos of galaxies and clusters (Bîrzan et al. 2004; Dunn et al. 2005; Rafferty et al. 2006).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, methodology): “%) of cavities (Dunn et al. 2005) and radio emission (Burns 1990) in cooling flow clusters further implicates AGN, although heat conduction or other agents may augment AGN heating (Ruszkowski & Begelman 2002; Brighenti & Mathews 2003).”
What drives the growth of black holes (2011, background): “…timescale for the lifetime of the radio source (for example from the buoyant rise time of the inflated bubble), we can then estimate the total mechanical power Pmech output by the AGN (e.g., Bı̂rzan et al., 2004; Dunn et al., 2005; Dunn & Fabian, 2008; Bı̂rzan et al., 2008; Cavagnolo et al., 2010).”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, background): “…2006; Allen et al. 1992) and/or interactions between central radio sources and the surrounding intracluster gas (e.g., Böhringer et al. 1993; Fabian et al. 2000, 2003, 2006; Birzan et al. 2004; Dunn & Fabian 2004; Forman et al. 2005; Dunn et al. 2005; Rafferty et al. 2006; Allen et al. 2006).”
Jet-induced star formation in gas-rich galaxies (2011, background): “…also is meanwhile considerable evidence from observations of X-ray cavities that the energies deposited by the jets suffice in many cases to suppress the formation of cooling flows in the hot circum-galactic and intra-cluster media (e.g. B̂ırzan et al. 2004; Dunn et al. 2005; Rafferty et al. 2006).”
Investigating AGN heating in a sample of nearby clusters (2006, methodology): “The energies and time-scales for the bubbles were calculated from values for the radii in Allen et al. (2006), Dunn et al. (2005), Dunn & Fabian (2004), except for 2A 0335+096 which are from Bı̂rzan et al. (2004).”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “Further cavity power measurements in systems ranging from giant elliptical galaxies to the most massive clusters have refined this correlation (e.g. Dunn et al. 2005, Rafferty et al. 2006, Bı̂rzan et al. 2008, Cavagnolo et al. 2010; see Fig.8).”
Filaments, Bubbles, and Weak Shocks in the Gaseous Atmosphere of M87 (2006, background): “Dunn et al. (2005) showed that buoyant bubbles may be a significant heat source in 70% of a sample of cooling core clusters (see also Birzan et al. 2004).”
A very deep Chandra observation of the Perseus cluster: shocks, ripples and conduction (2005, background): “This means that any estimate of bubbling power based simply on buoyancy times (e.g. Birzan et al 2004; Dunn et al 2004, 2005a) is a lower limit.”