X-ray Spectroscopy of Cooling Clusters

By J. R. Peterson, A. C. Fabian. 2005

422 citations recorded by the source corpus.

We review the X-ray spectra of the cores of clusters of galaxies. Recent high resolution X-ray spectroscopic observations have demonstrated a severe deficit of emission at the lowest X-ray temperatures as compared to that expected from simple radiative cooling models. The same observations have provided compelling evidence that the gas in the cores is cooling below half the maximum temperature. We review these results, discuss physical models of cooling clusters, and describe the X-ray instrumentation and analysis techniques used to make these observations. We discuss several viable mechanisms designed to cancel or distort the expected process of X-ray cluster cooling.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/40b8faf025fa811ee2f92a037a189d2c7178dfd6

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

In Instrumentation

Citations in the corpus

Raining on black holes and massive galaxies: the top-down multiphase condensation model (2016, background): “…radiative emissivity, the net cooling rate reaches a quasi-stable configuration at Ṁcool 1 M yr−1, which is more than 1 dex lower than that of the pure cooling flow model (Section 3.1), consistently with observed X-ray spectra (e.g. Peterson & Fabian 2006; Gaspari 2015 and references therein).”
Galaxy clustering in the CFHTLS-Wide: the changing relationship between galaxies and haloes since z ~ 1.2 (2011, methodology): “Several methodologies exist to estimate halo masses: for example, using satellite kinematics (More et al. 2011), X-ray temperatures (Peterson & Fabian 2006; Cattaneo et al. 2009), or gravitational lensing (Heymans et al. 2006; Mandelbaum et al. 2006; Auger et al. 2010; Leauthaud et al. 2012b).”
CAUSE AND EFFECT OF FEEDBACK: MULTIPHASE GAS IN CLUSTER CORES HEATED BY AGN JETS (2011, background): “All the features of the pure CF model, discussed above, are in contrast with observations of galaxy clusters (Peterson et al. 2001, 2003; Ettori et al. 2002; Tamura et al. 2003; Peterson & Fabian 2006).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “In particular, clusters for which radiative cooling in the core is efficient form an easily distinguishable subpopulation with significantly enhanced central gas density and luminosity, also commonly accompanied by a drop in ICM temperature (Fabian et al. 1994; Peterson & Fabian 2006).”
Feedback heating by cosmic rays in clusters of galaxies (2007, background): “…show that while the temperature is declining toward the center, there is a remarkable lack of emission lines from the gas at temperature below about ∼ 1/3 of the ambient cluster temperature (e.g., Peterson et al. (2001, 2003); Tamura et al. (2001); for a review see Peterson & Fabian (2006)).”
ON THE ORIGIN OF THE EXTENDED Hα FILAMENTS IN COOLING FLOW CLUSTERS (2010, methodology): “Mechanical and radiative feedback from active galactic nuclei (AGNs) and starbursts (e.g., Peterson & Fabian 2006; Veilleux et al. 2005), gas sloshing in the cluster core (e.g., ZuHone et al. 2010), merger shocks (e.g., Randall et al. 2002), and conduction from the surrounding ICM (e.g., Voigt &…”
Chaotic cold accretion on to black holes (2013, background): “Spectroscopic data show that the cooling rates are severely quenched (Peterson & Fabian 2006) and the global thermal equilibrium is likely maintained at an ∼10 per cent level.”
Diffuse Radio Emission from Galaxy Clusters (2019, background): “In the absence of a heating source, a cooling flow is expected to develop, whereby the tem- perature in the central region of the cluster drops and gas flows inwards (e.g., Fabian 1994; Peterson & Fabian 2006; Fabian 2012; McNamara & Nulsen 2012).”
An Entropy Threshold for Strong Hα and Radio Emission in the Cores of Galaxy Clusters (2008, background): “INTRODUCTION In recent years the “cooling flow problem” has been the focus of intense scrutiny as the solutions have broad impact on our theories of galaxy formation (see Peterson & Fabian 2006 for a review).”
A deeper X‐ray study of the core of the Perseus galaxy cluster: the power of sound waves and the distribution of metals and cosmic rays (2007, result): “Similar behaviour is found in many X-ray peaked, cool-core clusters (see Peterson & Fabian 2006, for a review).”
Mechanical AGN feedback: controlling the thermodynamical evolution of elliptical galaxies (2012, background): “Excellent reviews on this subject are provided by Peterson & Fabian (2006), McNamara & Nulsen (2007) and Böhringer & Werner (2010).”
How special are Brightest Group and Cluster Galaxies (2006, background): “Recent Xray studies have furthermore demonstrated that the clustergas does not cool below∼ 2 keV (e.g. Peterson & Fabian 2006).”
Heating Hot Atmospheres with Active Galactic Nuclei (2007, background): “As outlined above, the constant pressure cooling model makes spe- cific predictions of the strengths of lines from low temperature cooling gas (cf. Böhringer et al. 2002; Peterson & Fabian 2006).”
Thermal instability and the feedback regulation of hot haloes in clusters, groups and galaxies (2011, background): “…more typically they show accretion rates between 1 and 10 M⊙ yr −1, in broad agreement with accretion rates inferred from X-ray spectral modeling (see Peterson & Fabian 2006 for a review on X-ray spectroscopy of clusters) and from the star formation rates in the central galaxy (e.g., O’Dea et…”
Investigating AGN heating in a sample of nearby clusters (2006, background): “However, with the high spatial and spectral resolution of Chandra and XMM–Newton little of the expected X-ray emitting cool gas has been found (Peterson et al. 2003, see Peterson & Fabian 2006 for a review).”