Systematic study of X-ray cavities in the brightest galaxy in the Draco constellation NGC 6338

Pandge, M. B.; Vagshette, N. D.; David, L. P.; Patil, M. K.

doi:10.1111/j.1365-2966.2011.20358.x

Cited by 38 publications

(56 citation statements)

References 43 publications

(88 reference statements)

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“…The evidences for the presence of such cavities were first reported from the ROSAT observations of Perseus cluster (Boehringer et al 1993). The availability of high quality data from Chandra observations of clusters and groups made it possible to detect many such cases and study their interaction with the ICM in detail (McNamara et al 2000;Fabian et al 2000;Sanders & Fabian 2002;Rafferty et al 2006;Fabian et al 2006;Bîrzan et al 2008;Dong et al 2010;Dunn et al 2010;O'Sullivan et al 2011;David et al 2009;Gitti et al 2012;Pandge et al 2013Pandge et al , 2012Sonkamble et al 2015;Vagshette et al 2016). Radio observations of several such clusters revealed that these cavities spatially match with the radio lobes and are filled with non-thermal gas consisting of relativistic particles and magnetic field (McNamara & Nulsen 2007;Gitti et al 2012).…”

Section: Introductionmentioning

confidence: 99%

“…It is well known that AGN feedback plays an important role in balancing cooling and heating of the ICM (Fabian 1994;McNamara et al 2005;Bîrzan et al 2004;Rafferty et al 2006;Doria et al 2012;Pandge et al 2012;Sonkamble et al 2015;Vagshette et al 2016). Power required to heat the ICM through AGN feedback can be derived by taking the ratio between the total energy required to create cavities in the ICM and the age of the cavity.…”

Section: Cavity Energeticsmentioning

confidence: 99%

See 1 more Smart Citation

Detection of a pair of prominent X-ray cavities in Abell 3847

Vagshette

Naik

Patil

et al. 2016

Mon. Not. R. Astron. Soc.

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We present results obtained from a detailed analysis of a deep Chandra observation of the bright FRII radio galaxy 3C 444 in Abell 3847 cluster. A pair of huge X-ray cavities are detected along North and South directions from the centre of 3C 444. X-ray and radio images of the cluster reveal peculiar positioning of the cavities and radio bubbles. The radio lobes and X-ray cavities are apparently not spatially coincident and exhibit offsets by ∼ 61 kpc and 77 kpc from each other along the North and South directions, respectively. Radial temperature and density profiles reveal the presence of a cool core in the cluster. Imaging and spectral studies showed the removal of substantial amount of matter from the core of the cluster by the radio jets. A detailed analysis of the temperature and density profiles showed the presence of a rarely detected elliptical shock in the cluster. Detection of inflating cavities at an average distance of ∼ 55 kpc from the centre implies that the central engine feeds a remarkable amount of radio power (∼6.3 ×10 44 erg s −1 ) into the intra-cluster medium over ∼ 10 8 yr, the estimated age of cavity. The cooling luminosity of the cluster was estimated to be ∼ 8.30 × 10 43 erg s −1 , which confirms that the AGN power is sufficient to quench the cooling. Ratios of mass accretion rate to Eddington and Bondi rates were estimated to be ∼ 0.08 and 3.5 × 10 4 , respectively. This indicates that the black hole in the core of the cluster accretes matter through chaotic cold accretion.

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Section: Introductionmentioning

confidence: 99%

Section: Cavity Energeticsmentioning

confidence: 99%

Detection of a pair of prominent X-ray cavities in Abell 3847

Vagshette

Naik

Patil

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Over the years the AGN feedback mechanism, mostly by jet-inflated bubbles, has been solidified (e.g., Dong et al 2010;O'Sullivan et al 2011;Farage et al 2012;Gaspari et al 2012a,b;Birzan et al 2011;Gitti et al 2012;Pfrommer 2013). Key to the establishment of the AGN-JFM in cooling flows are the many observations of X-ray deficient bubbles (e.g., Boehringer et al 1993;Fabian et al 2000;McNamara et al 2001;Heinz et al 2002;Forman et al 2007;Wise et al 2007;Baldi et al 2009;David et al 2009;Gastaldello et al 2009;Gitti et al 2010;Blanton et al 2011;David et al 2011;Machacek et al 2011;Randall et al 2011;Doria et al 2012;Pandge et al 2012;Hlavacek-Larrondo et al 2015). Many of these X-ray bipolar structures resemble visible bipolar structures observed in bipolar PNe (see Figs.…”

Section: Jet-inflated Bubblesmentioning

confidence: 99%

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Soker

2016

New Astronomy Reviews

149

106

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I review the influence jets and the bubbles they inflate might have on their ambient gas as they operate through a negative jet feedback mechanism (JFM). I discuss astrophysical systems where jets are observed to influence the ambient gas, in many cases by inflating large, hot, and low-density bubbles, and systems where the operation of the JFM is still a theoretical suggestion. The first group includes cooling flows in galaxies and clusters of galaxies, star-forming galaxies, young stellar objects, and bipolar planetary nebulae. The second group includes core collapse supernovae, the common envelope evolution, the grazing envelope evolution, and intermediate luminosity optical transients. The suggestion that the JFM operates in these four types of systems is based on the assumption that jets are much more common than what is inferred from objects where they are directly observed. Common to all eight types of systems reviewed here is the presence of a compact object inside an extended ambient gas. The ambient gas serves as a potential reservoir of mass to be accreted on to the compact object. If the compact object launches jets as it accretes mass, the jets might reduce the accretion rate as they deposit energy to the ambient gas, or even remove the entire ambient gas, hence closing a negative feedback cycle.

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“…This feedback mechanism is driven by active galactic nucleus (AGN) jets that inflate X-ray deficient cavities (bubbles; e.g., Dong et al 2010;O'Sullivan et al 2011;Gaspari et al 2012a,b;Gilkis & Soker 2012). Examples of bubbles in cooling flows include Abell 2052 (Blanton et al 2011), NGC 6338 (Pandge et al 2012), NGC 5044 (David et al 2009), and HCG 62 (Gitti et al 2010), among many others.…”

Section: Introductionmentioning

confidence: 99%

Heating the intracluster medium by jet-inflated bubbles

Hillel

Soker

2015

Mon. Not. R. Astron. Soc.

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We examine the heating of the intra-cluster medium (ICM) of cooling flow clusters of galaxies by jet-inflated bubbles and conclude that mixing of hot bubble gas with the ICM is more important than turbulent heating and shock heating. We use the pluto hydrodynamical code in full 3D to properly account for the inflation of the bubbles and to the multiple vortices induced by the jets and bubbles. The vortices mix some hot shocked jet gas with the ICM. For the parameters used by us the mixing process accounts for about four times as much heating as that by the kinetic energy in the ICM, namely, turbulence and sound waves. We conclude that turbulent heating plays a smaller role than mixing. Heating by shocks is even less efficient.

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Systematic study of X-ray cavities in the brightest galaxy in the Draco constellation NGC 6338

Cited by 38 publications

References 43 publications

Detection of a pair of prominent X-ray cavities in Abell 3847

Detection of a pair of prominent X-ray cavities in Abell 3847

The jet feedback mechanism (JFM) in stars, galaxies and clusters

Heating the intracluster medium by jet-inflated bubbles

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