2004
DOI: 10.1111/j.1365-2966.2004.07285.x
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Thermal conduction and reduced cooling flows in galaxy clusters

Abstract: Conduction may play an important role in reducing cooling flows in galaxy clusters. We analyse a sample of sixteen objects using Chandra data and find that a balance between conduction and cooling can exist in the hotter clusters (T > 5 keV), provided the plasma conductivity is close to the unhindered Spitzer value. In the absence of any additional heat sources, a reduced mass inflow must develop in the cooler objects in the sample. We fit cooling flow models to deprojected data and compare the spectral mass d… Show more

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Cited by 218 publications
(297 citation statements)
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“…Therefore, the relative importance of conductive to AGN heating is largely determined by the temperature profile and the mass of the clusters. Previous works have tried to evaluate the importance of conductive heating from the observed profiles of clusters assuming one-third of Spitzer conductivity (e.g., Voigt & Fabian 2004;Voit 2011). Our results suggest that there indeed exists a quasi-steady thermal balance among cooling, AGN feedback, and conduction (Voit 2011), and the contributions from conduction and AGN heating derived from such observations should not vary more than a factor of a few over the course of the cluster evolution once their cores have reached such a quasi-equilibrium stage.…”
Section: Discussionmentioning
confidence: 99%
See 1 more Smart Citation
“…Therefore, the relative importance of conductive to AGN heating is largely determined by the temperature profile and the mass of the clusters. Previous works have tried to evaluate the importance of conductive heating from the observed profiles of clusters assuming one-third of Spitzer conductivity (e.g., Voigt & Fabian 2004;Voit 2011). Our results suggest that there indeed exists a quasi-steady thermal balance among cooling, AGN feedback, and conduction (Voit 2011), and the contributions from conduction and AGN heating derived from such observations should not vary more than a factor of a few over the course of the cluster evolution once their cores have reached such a quasi-equilibrium stage.…”
Section: Discussionmentioning
confidence: 99%
“…First, thermal conduction has the potential to be extremely important for the thermodynamic state of a CC (e.g., Voigt & Fabian 2004;Voit 2011). While it cannot by itself offset the radiative cooling in a stable manner (Stewart et al 1984;Bregman & David 1988;Soker 2003;Zakamska & Narayan 2003;Voigt & Fabian 2004;Pope et al 2006), it may provide part of the heating, reducing the burden on the AGN, and can aid in the isotropization of the AGN heating throughout the core. Second, the ICM is known to be magnetized with β∼100 (Carilli & Taylor 2002), where β is defined as the ratio between gas thermal pressure and magnetic pressure.…”
Section: Introductionmentioning
confidence: 99%
“…This has led to the conclusion that star formation is fueled in the BCG by residual cooling flows (Voigt & Fabian 2004;Tremblay et al 2012;McDonald et al 2014b). In order to test whether this trend was established at high-z, we require estimates of the core entropy and cooling rate for each cluster.…”
Section: X-ray Analysis: Central Entropy and Luminositymentioning
confidence: 99%
“…In order to test whether this trend was established at high-z, we require estimates of the core entropy and cooling rate for each cluster. Given that we only have ∼2000 X-ray counts per cluster, modeling the central entropy (e.g., Cavagnolo et al 2009) or estimating the spectroscopically derived cooling rate (e.g., Voigt & Fabian 2004) is not feasible. Instead, we compute spectroscopic quantities (bolometric luminosity, temperature) from a circular aperture with a radius of 0.075 R 500 (where R 500 was derived based on the Y X -M 500 relation of Vikhlinin et al 2009), which should roughly correspond to the deprojected core temperature (see e.g., McDonald et al 2014a).…”
Section: X-ray Analysis: Central Entropy and Luminositymentioning
confidence: 99%
“…conduction (Zakamska & Narayan 2003;Voigt & Fabian 2004), turbulent mixing (Kim & Narayan 2003), mergers (Gómez et al 2002), sloshing (ZuHone et al 2010), SN (Domainko et al 2004), turbulence energy triggered by SF and SN (FalcetaGonçalves et al 2010;de Gouveia Dal Pino et al 2011), and gravitational heating from clumpy accretion (Dekel & Birnboim 2008).…”
Section: Introductionmentioning
confidence: 99%