X-ray spectroscopy of cooling clusters

Peterson, J. R.; Fabian, A. C.

doi:10.1016/j.physrep.2005.12.007

Cited by 541 publications

(603 citation statements)

References 231 publications

(76 reference statements)

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“…In fact, the luminosity of any particular X-ray emission line is simply given by the energy injected into the plasma by its passage across the shock front multiplied by the fraction of the total plasma emissivity that is due to that line (Gayley 2014) -a result we derive below in detail (and ultimately show in equation 7). We note the similarity to the treatment of X-ray emission from cooling flows in galaxy clusters (Peterson & Fabian 2006). Furthermore, since plasma impulsively heated to a given temperature as it crosses a shock front will radiate at that temperature and, as time goes on, at every lower temperature until it is fully cooled, an emission line that forms at a given temperature will probe shocks of every higher temperature.…”

Section: Introductionmentioning

confidence: 60%

Measuring the shock-heating rate in the winds of O stars using X-ray line spectra

Cohen

Gayley

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present a new method for using measured X-ray emission line fluxes from O stars to determine the shock-heating rate due to instabilities in their radiation-driven winds. The high densities of these winds means that their embedded shocks quickly cool by local radiative emission, while cooling by expansion should be negligible. Ignoring for simplicity any non-radiative mixing or conductive cooling, the method presented here exploits the idea that the cooling post-shock plasma systematically passes through the temperature characteristic of distinct emission lines in the X-ray spectrum. In this way, the observed flux distribution among these X-ray lines can be used to construct the cumulative probability distribution of shock strengths that a typical wind parcel encounters as it advects through the wind. We apply this new method to Chandra grating spectra from five O stars with X-ray emission indicative of embedded wind shocks in effectively single massive stars. The results for all the stars are quite similar: the average wind mass element passes through roughly one shock that heats it to at least 10 6 K as it advects through the wind, and the cumulative distribution of shock strengths is a strongly decreasing function of temperature, consistent with a negative power-law of index n ≈ 3, implying a marginal distribution of shock strengths that scales as T −4 , and with hints of an even steeper decline or cut-off above 10 7 K.

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Section: Introductionmentioning

confidence: 60%

Measuring the shock-heating rate in the winds of O stars using X-ray line spectra

Cohen

Gayley

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…This amount of energy released (called the AGN feedback) is sufficient to balance the cooling of hot atmosphere surrounding the central engine (Bîrzan et al 2004;Best et al 2006;Dunn & Fabian 2006;Rafferty et al 2006;Bîrzan et al 2009;Dong et al 2010;Vagshette et al 2016). Apart from AGN feedback, there are other possible heating mechanisms as proposed by several authors; like heating due to merging (Peterson & Fabian 2006;, supernovae heating (Domainko et al 2004), cosmic rays heating (Colafrancesco et al 2004;Totani 2004), etc. However, AGN feedback mechanism provides the most acceptable explanation for heating the ICM.…”

Section: Introductionmentioning

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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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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“…In this process the gas density increases at the core and further boosts the X-ray emission, as the X-ray emissivity is proportional to the square of the gas density (Sarazin 1988). This cooling flow will produce a strong surface brightness peak toward the centre of clusters and a drop in temperature in the core (Peterson & Fabian 2006). This classical picture does not consider any heating mechanism, which must be in place, because X-ray observations of galaxy clusters by Chandra and XMM-Newton show no sign of gas temperatures below ∼ keV.…”

Section: Introductionmentioning

confidence: 99%

IGM heating in fossil galaxy groups

Miraghaei

Khosroshahi

Klöckner

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We study intergalactic medium (IGM) heating in a sample of five fossil galaxy groups by using their radio properties at 610 MHz and 1.4 GHz. The power by radio jets introducing mechanical heating for the sampled objects is not sufficient enough to suppress the cooling flow. Therefore, we discussed shock-, vortex heating, and conduction as alternative heating processes. Further, the 1.4 GHz and 610 MHz radio luminosities of fossil groups are compared to a sample of normal galaxy groups of the same radio brightest (BGGs), stellar mass, and total group stellar mass, quantified using the K-band luminosity. It appears that the fossil BGGs are under luminous at 1.4 GHz and 610 MHz for a given BGG stellar mass and luminosity, in comparison to a general population of the groups. In addition, we explore how the bolometric radio luminosity of fossil sample depends on clusters and groups characteristics. Using the HIghest X-ray FLUx Galaxy Cluster Sample (HIFLUGCS) as a control sample we found that the large-scale behaviours of fossil galaxy groups are consistent with their relaxed and virialised nature.

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X-ray spectroscopy of cooling clusters

Cited by 541 publications

References 231 publications

Measuring the shock-heating rate in the winds of O stars using X-ray line spectra

Measuring the shock-heating rate in the winds of O stars using X-ray line spectra

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

IGM heating in fossil galaxy groups

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