THE EVOLUTION OF X-RAY CLUSTERS OF GALAXIES

By Piero Rosati, Stefano Borgani, C. Norman. 2002

391 citations recorded by the source corpus.

■ Abstract Considerable progress has been made over the past decade in the study of the evolutionary trends of the population of galaxy clusters in the Universe. In this review we focus on observations in the X-ray band. X-ray surveys with the ROSAT satellite, supplemented by follow-up studies with ASCA and Beppo-SAX, have allowed an assessment of the evolution of the space density of clusters out to z 1 and the evolution of the physical properties of the intracluster medium out to z 0.5. With the advent of Chandra and Newton-XMM and their unprecedented sensitivity and angular resolution, these studies have been extended beyond redshift unity and have revealed the complexity of the thermodynamical structure of clusters. The properties of the intracluster gas are significantly affected by nongravitational processes including star formation and Active Galactic Nuclei (AGN) activity. Convincing evidence has emerged for modest evolution of both the bulk of the X-ray cluster population and their thermodynamical properties since redshift unity. Such an observational scenario is consistent with hierarchical models of structure formation in a flat low-density

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/afa476bd149bdfbfe79741db288edee890609a53

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

DEEP EXTRAGALACTIC X-RAY SURVEYS (2005, background): “In the 5–10 keV band a flattening has not yet been detected; the faint-end number counts continue rising steeply (αf ≈ 1.2–1.4) indicating that a significant fraction of the 5–10 keV CXRB remains unresolved (e.g., Rosati et al. 2002b).”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, methodology): “A comparison of the efficiency of detecting clusters in X-rays versus other methods can be found, for example, in Rosati et al. (2002).”
A mature cluster with X-ray emission at z = 2.07 (2010, background): “…and thermodynamical evolution of the X-ray shining ICM within their deep potential wells and the build-up of their constituent galaxy population must then be addressedby looking as closely as possible at the early stages of their formation (Voit 2005, Ponman et al. 1999, Rosati et al. 2002).”
Catalog extraction in SZ cluster surveys : a matched filter approach (2006, background): “…features, such as the recently detected baryon oscillations (Eisenstein et al. 2005; Cole et al. 2005; Angulo et al. 2005; Huetsi 2006), and provide a sensitive gauge of structure growth back to high redshifts (Oukbir & Blanchard 1992; Rosati et al. 2002; Voit 2004, and references therein).”
EVOLUTION OF THE COLOR–MAGNITUDE RELATION IN GALAXY CLUSTERS AT z ∼ 1 FROM THE ACS INTERMEDIATE REDSHIFT CLUSTER SURVEY (2008, background): “…458, 717 Rosati et al. 1998, ApJ, 492, L21 Rosati, P., Stanford, S.A., Eisenhardt, P.R., Elston, R., Spinrad, H., Stern, D., Dey, A. 1999, ApJ, 118, 76 Rosati et al. 2002, ARA&A, 40, 539 Rosati, P. et al., 2004, AJ, 127, 230 Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525…”
Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey (2008, background): “14 There is no generally agreed on definition for galaxy clusters: see, e.g., Abell (1958), Postman et al. (1996), and Rosati et al. (2002).”
A SPITZER-SELECTED GALAXY CLUSTER AT z = 1.62 (2010, background): “…al. 2004; Stanford et al. 2006), but X–ray selection typically require relaxed systems, which is unlikely to be the case at high redshifts where cluster progenitors will be less massive and more disordered, with less time for the intracluster medium (ICM) to thermalize (e.g., Rosati et al. 2002).”
The XMM-Newton Wide-Field Survey in the COSMOS Field: Statistical Properties of Clusters of Galaxies (2006, methodology): “We note that the prediction for no evolution in the luminosity function obtained by local surveys, as summarized in Rosati et al. (2002), provides a good fit to our cluster counts.”
The SRG/eROSITA all-sky survey (2024, neutral): “…geometry and growth history of the cosmos, and therefore prime cosmological tools (Bahcall 1977; Cavaliere & Fusco-Femiano 1978; Sarazin 1986; Rosati et al. 2002; Voit 2005; Arnaud 2005; Norman 2005; Borgani 2008; Vikhlinin et al. 2009; Borgani & Kravtsov 2011; Allen et al. 2011; Reiprich et…”
RESIDUAL GAS MOTIONS IN THE INTRACLUSTER MEDIUM AND BIAS IN HYDROSTATIC MEASUREMENTS OF MASS PROFILES OF CLUSTERS (2009, neutral): “Traditionally, the masses are estimated using observable X-ray properties of the intracluster plasma using spectroscopic X-ray temperature or luminosity (e.g., Rosati et al. 2002, for a review) or velocity dispersion of cluster galaxies.”
On the efficiency and reliability of cluster mass estimates based on member galaxies (2006, background): “The number density of clusters of galaxies abovea given mass threshold, and the evolution of this abundance with redshiftz, provides in principle strong constraints on cosmological models/parameters (see, e.g., Rosati et al. 2002; Voit 2005, for recent reviews, and references therein).”
Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3 (2003, background): “…of vital importance if the evolution of the cluster population has to be used as a proxy to the cosmic evolution and, therefore, for the determination of cosmological parameters (e.g., the pioneering work of Henry & Arnaud 1991; see Rosati et al. 2002, for a recent review and references therein).”
Systematics in the X-ray cluster mass estimators (2006, background): “At the present, statistical uncertainties associated to the paucity of available high-redshift cluster samples are comparable to systematic uncertainties arising from biases in cluster mass estimates (see e.g. Rosati et al. 2002), as those discussed in this paper.”