Heating versus Cooling in Galaxies and Clusters of Galaxies

1. Front Matter

   Pages I-XXIII

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2. Observations of Cooling Cores

   1. Front Matter

      Pages 1-1

      PDF

   2. Introduction to Cluster Cooling Cores

      • C.L. Sarazin

      Pages 3-12

   3. Star Formation and Feedback in Cooling Flows

      • B. R. McNamara

      Pages 13-19

   4. Cold Gas in Cluster Cores

      • M. Donahue

      Pages 20-29

   5. Statistics of X-ray Observables of Cooling Core and Non-cooling Core Clusters of Galaxies

      • Y. Chen, T.H. Reiprich, H. Böhringer, Y. Ikebe

      Pages 30-32

   6. Cold Fronts in Cool Core Clusters

      • S. Ghizzardi, S. Molendi, M. Rossetti, A. Leccardi

      Pages 33-38

   7. Core structure of Intracluster Gas: Effects of Radiative Cooling on Core Sizes

      • T. Akahori, K. Masai

      Pages 39-41

   8. Investigating the Central Regions of the HIFLUGCS Clusters with Chandra

      • D. S. Hudson, T. H. Reiprich

      Pages 42-44

   9. Investigating Heating and Cooling within a Sample of Distant Clusters

      • R.J.H. Dunn, A.C. Fabian

      Pages 45-47

   10. Lack of Cooling Flow Clusters at z > 0.5

       • A. Vikhlinin, R. Burenin, W. R. Forman, C. Jones, A. Hornstrup, S. S. Murray et al.

       Pages 48-53

   11. The XDCP Prospects of Finding Cooling Core Clusters at Large Lookback Times

       • R. Fassbender, H. Böhringer, J. Santos, P. Schuecker, G. Lamer, A. Schwope et al.

       Pages 54-56

   12. An XMM-Newton View of Three Clusters of Galaxies

       • T.F. Laganá, G.B. Lima Neto, F. Durret

       Pages 57-59

   13. Exploring Massive Galaxy Clusters: XMM-Newton observations of two morphology unbiased samples at z ∼ 0.2 and z ∼ 0.3

       • Y.-Y. Zhang, A. Finoguenov, H. Böhringer, J.-P. Kneib, G. P. Smith, O. Czoske et al.

       Pages 60-62

3. AGN-ICM Interaction in Cool Cores

   1. Front Matter

      Pages 63-63

      PDF

   2. Heating and Cooling in the Perseus Cluster Core

      • A.C. Fabian, J.S. Sanders

      Pages 65-73

   3. Hard X-ray emission from the core of the Perseus cluster and the thermal content of the radio bubbles

      • J.S. Sanders, A.C. Fabian

      Pages 74-79

   4. Outbursts from Supermassive Black Holes: Shocks, Bubbles, and Filaments Around M87

      • W. Forman, E. Churazov, C. Jones, P. Nulsen, R. Kraft, H. Böhringer et al.

      Pages 80-86

   5. The Gaseous Atmosphere of M87 seen with XMM-Newton

      • A. Simionescu, H. Böhringer, M. Brüggen, A. Finoguenov

      Pages 87-89

   6. The XMM-Newton View of MS0735+7421: the Most Energetic AGN Outburst in a Galaxy Cluster

      • M. Gitti, B. R. McNamara, P.E.J. Nulsen, M. W. Wise

      Pages 90-94

The Universe would be a dull and dark place if the gaseous baryons did not cool, collapse, and form stars and galaxies. However, if this gas is allowed to cool unimpeded at the rate predicted from known atomic physics, in the context of a well-established cosmological model, the gaseous matter would form stars and galaxies with a high e?ciency, so that far more than the observed fraction of about 10–15% of the baryonic matter would be found in luminous stellar systems. Therefore,cooling must be damped or regulatedby heating processes, and observations show that this ‘feedback’ is a widespread astrophysical phenomenon. The place where this cooling and feedback manifests itself most dram- ically is in the inner regions of the most massive Dark Matter halos found in our Universe, in the cores of galaxy clusters. The e?ect of cosmic co- ing in these objects was recognized in the mid-1970s, and the term ‘cooling ?ow’ was introduced by Andy Fabian and colleagues at Cambridge as a p- sible explanation of the physical processes obtained in the central regions of clusters. The name refers to the fact that gas cooling in the inner regions is associated with a loss of central pressure, causing an in?ow of hot gas from larger radii.

• Astrophysical Cooling Cores
• Cluster Cooling Cores
• Cosmic Structure Formation
• Galaxy
• Galaxy Clusters
• Galaxy Formation
• astronomy

• Max-Planck-Institut, für extraterrestrische Physik, Giessenbachstraβe, Germany

  H. Böhringer, G.W. Pratt, A. Finoguenov, P. Schuecker

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