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Space Science Reviews

, 215:25 | Cite as

The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population

  • G. W. PrattEmail author
  • M. Arnaud
  • A. Biviano
  • D. Eckert
  • S. Ettori
  • D. Nagai
  • N. Okabe
  • T. H. Reiprich
Article
Part of the following topical collections:
  1. Clusters of Galaxies: Physics and Cosmology

Abstract

The total mass of a galaxy cluster is one of its most fundamental properties. Together with the redshift, the mass links observation and theory, allowing us to use the cluster population to test models of structure formation and to constrain cosmological parameters. Building on the rich heritage from X-ray surveys, new results from Sunyaev-Zeldovich and optical surveys have stimulated a resurgence of interest in cluster cosmology. These studies have generally found fewer clusters than predicted by the baseline Planck\(\varLambda\)CDM model, prompting a renewed effort on the part of the community to obtain a definitive measure of the true cluster mass scale. Here we review recent progress on this front. Our theoretical understanding continues to advance, with numerical simulations being the cornerstone of this effort. On the observational side, new, sophisticated techniques are being deployed in individual mass measurements and to account for selection biases in cluster surveys. We summarise the state of the art in cluster mass estimation methods and the systematic uncertainties and biases inherent in each approach, which are now well identified and understood, and explore how current uncertainties propagate into the cosmological parameter analysis. We discuss the prospects for improvements to the measurement of the mass scale using upcoming multi-wavelength data, and the future use of the cluster population as a cosmological probe.

Keywords

Galaxy clusters Large-scale structure of the Universe Intracluster matter Cosmological parameters 

Notes

Acknowledgements

This work was initiated during a visit to the International Space Science Institute (ISSI) in Bern and we acknowledge ISSI’s hospitality. GWP and MA acknowledge funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 340519. SE acknowledges financial contribution from the contracts NARO15 ASI-INAF I/037/12/0, ASI 2015-046-R.0, ASI-INAF n.2017-14-H.0 and funding from the European Union’s Horizon 2020 Programme under the AHEAD project (grant agreement n. 654215). DN acknowledges Yale University for granting a triennial leave and the Max-Planck-Institut für Astrophysik for hospitality when this work was carried out. THR acknowledges support from the German Aerospace Agency (DLR) with funds from the Ministry of Economy and Technology (BMWi) through grant 50 OR 1514.

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Copyright information

© Springer Nature B.V. 2019

Authors and Affiliations

  • G. W. Pratt
    • 1
    Email author
  • M. Arnaud
    • 1
  • A. Biviano
    • 2
  • D. Eckert
    • 3
  • S. Ettori
    • 4
  • D. Nagai
    • 5
    • 6
  • N. Okabe
    • 7
  • T. H. Reiprich
    • 8
  1. 1.AIM, CEA, CNRS, Université Paris-SaclayUniversité Paris Diderot, Sorbonne Paris CitéGif-sur-YvetteFrance
  2. 2.INAF-Osservatorio Astronomico di TriesteTriesteItaly
  3. 3.Max-Planck-Institut für extraterrestrische PhysikGarchingGermany
  4. 4.INAF-Osservatorio di Astrofisica e Scienza dello SpazioBolognaItaly
  5. 5.Department of PhysicsYale UniversityNew HavenUSA
  6. 6.Yale Center for Astronomy and AstrophysicsNew HavenUSA
  7. 7.Department of Physical ScienceHiroshima UniversityHigashi-HiroshimaJapan
  8. 8.Argelander Institute for AstronomyUniversity of BonnBonnGermany

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