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.
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Notes
Existing experimental constraints and future prospects on gas motions in the ICM are discussed in detail in another chapter of this series (Simionescu et al. 2019).
Note that because of this choice these constraints are tighter than the ones shown in Schellenberger and Reiprich (2017b).
For more details, see the review by Mroczkowski et al. (2019, in this issue).
Measurements will also be possible in the outskirts of high-redshift clusters using high-resolution SZ spectral imaging observations through tSZ pressure fluctuations and direct kSZ measurements of internal gas motions (see the review by Mroczkowski et al. 2019, in this issue).
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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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Pratt, G.W., Arnaud, M., Biviano, A. et al. The Galaxy Cluster Mass Scale and Its Impact on Cosmological Constraints from the Cluster Population. Space Sci Rev 215, 25 (2019). https://doi.org/10.1007/s11214-019-0591-0
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DOI: https://doi.org/10.1007/s11214-019-0591-0