Searching for cool core clusters at high redshift

By Joana S. Santos, Piero Rosati, P. Tozzi, H. Boehringer, S. Ettori, A. F. M. F. E. Physik, E. Observatory, Inaf - Trieste, I. Bologna. 2008

158 citations recorded by the source corpus.

Aims. We investigate the detection of Cool Cores (CCs) in the distant galaxy cluster population with the purpose of measuring the CC fraction out to redshift 0.7 ≤ z 0.7, and should also be related to the shorter age of distant clusters, implying less time to develop a cool core.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4a41a6c4fdaf8617ff3435555cd225adf837c763

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Citations in the corpus

What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample (2009, methodology): “Recently Santos et al. (2008) compared a nearby sample of 11 clusters (z= 0.15− 0.3) to a distant sample of 15 clusters (z= 0.7− 1.4).”
ON THE CONNECTION BETWEEN GIANT RADIO HALOS AND CLUSTER MERGERS (2010, methodology): “…al. 2005; Ventimiglia et al. 2008; Böhringer et al. 2010); the emission centroid shift (e.g., Mohr et al. 1993; Poole et al. 2006, O’Hara et al. 2006; Ventimiglia et al. 2008, Maughan et al. 2008, Böhringer et al. 2010) and the surface brightness concentration parameter (e.g., Santos et al 2008).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “Cool cores are also common in X-ray selected samples at high redshift (Santos et al. 2008; 0.7 < z < 1.4).”
X-ray–optical classification of cluster mergers and the evolution of the cluster merger fraction (2011, background): “…of fully relaxed clusters decreases dramatically with look-back time even within the limited redshift range of our sample, lending strong support to previous claims of a pronounced dearth of cool-core clusters at high redshift (Vikhlinin et al. 2007; Santos et al. 2008; Samuele et al. 2011).”
The cluster gas mass fraction as a cosmological probe: a revised study (2009, background): “This follows recent evidence that cooling cores, at relativly higher central density, preferentially form later in time (e.g. Santos et al. 2008; Ettori & Brighenti 2008).”
ON THE ORIGIN OF THE EXTENDED Hα FILAMENTS IN COOLING FLOW CLUSTERS (2010, background): “Interestingly, recent studies have shown that beyond z ∼ 0.5 the frequency of clusters with cool cores is significantly lower than in the local universe (see e.g., Vikhlinin et al. 2007; Santos et al. 2008).”