2010
DOI: 10.1051/0004-6361/200912377
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Abstract: We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. In order to identify the best parameter for characterizing cool-core clusters and quantify its relation to other parameters, we mainly use very high spatial resolution profiles of central gas density and temperature, and quantities derived from them. We also correlate optical properties of brightest… Show more

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Cited by 410 publications
(646 citation statements)
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References 134 publications
(238 reference statements)
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“…For the ACCEPT (Cavagnolo et al 2009) and CLASH ) samples, we apply a small correction because both of these cluster samples are biased toward cool core clusters. This bias correction assumes that the true, underlying fraction of cool core clusters is 30% (Haarsma et al 2010;Hudson et al 2010;McDonald et al 2013b) and that non-cool cores do not have star-forming BCGs at z0.5 (Cavagnolo et al 2008;O'Dea et al 2008;McDonald et al 2010). This well-motivated correction brings the observed Figure 3.…”
Section: The Evolving Fraction Of Star-forming Bcgsmentioning
confidence: 99%
See 1 more Smart Citation
“…For the ACCEPT (Cavagnolo et al 2009) and CLASH ) samples, we apply a small correction because both of these cluster samples are biased toward cool core clusters. This bias correction assumes that the true, underlying fraction of cool core clusters is 30% (Haarsma et al 2010;Hudson et al 2010;McDonald et al 2013b) and that non-cool cores do not have star-forming BCGs at z0.5 (Cavagnolo et al 2008;O'Dea et al 2008;McDonald et al 2010). This well-motivated correction brings the observed Figure 3.…”
Section: The Evolving Fraction Of Star-forming Bcgsmentioning
confidence: 99%
“…Numerous studies have found evidence for ultraviolet (UV) and infrared (IR) continuum (e.g., McNamara & O'Connell 1989;Hicks & Mushotzky 2005;O'Dea et al 2008;McDonald et al 2011b;Hoffer et al 2012;Rawle et al 2012;Fraser-McKelvie et al 2014;Donahue et al 2015), warm, ionized gas (e.g., Hu et al 1985;Johnstone et al 1987;Heckman et al 1989;Crawford et al 1999;Edwards et al 2007;Hatch et al 2007;McDonald et al 2010McDonald et al , 2011a, and both warm and cold molecular gas (e.g., Jaffe & Bremer 1997;Donahue et al 2000;Edge 2001;Edge et al 2002;Edge & Frayer 2003;Salomé & Combes 2003;Hatch et al 2005;Jaffe et al 2005;Johnstone et al 2007;Oonk et al 2010;McDonald et al 2012c)-all of which are indicative of ongoing or recent star formation. Star-forming BCGs were found preferentially in galaxy clusters with "cool cores," as identified by a central density enhancement in the ICM (e.g., Vikhlinin et al 2007;Santos et al 2008;Hudson et al 2010) or low central entropy/cooling time (e.g., Cavagnolo et al 2008Cavagnolo et al , 2009Hudson et al 2010). These and other works established a link between the cooling ICM and the presence of multiphase gas, suggesting that cooling flows may indeed be fueling star formation in BCGs.…”
Section: Introductionmentioning
confidence: 99%
“…For instance, Hudson et al (2010) and Mittal et al (2011) showed that due to the enhanced L X for a given T X (or M ), clusters with cool cores are overrepresented in an X-ray survey. Similarly, Eckert et al (2011) showed that the detection efficiency of X-ray instruments is not the same for centrally peaked (CC) and flat (NCC) objects; they quantified this dependence on the surface brightness and corrected the corresponding fractions.…”
Section: Some General Considerationsmentioning
confidence: 99%
“…By definition, cool-core clusters are characterised by relatively cold gas with high mass-deposition rates at their centres (see Hudson et al 2010 for a review). This builds up a reservoir of cold gas for the BCGs at their centres, which may feed the AGN and provide fuel to the radio emission.…”
Section: Bcgs Accretion and The Radio Properties Of The Host Clustersmentioning
confidence: 99%