On the Tension between Large Scale Structures and Cosmic Microwave Background - INSPIRE

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On the Tension between Large Scale Structures and Cosmic Microwave Background

Sep 13, 2018

5 pages

Part of Proceedings, 2nd World Summit on Exploring the Dark Side of the Universe (EDSU2018) : Point a Pitre, Guadeloupe, France, June 25-29, 2018, 037

Published in:

PoS EDSU2018 (2018) 037

Contribution to:

- EDSU2018
, 037

Published: Sep 13, 2018 by SISSA

e-Print:

1901.05289 [astro-ph.CO]

DOI:

10.22323/1.335.0037

View in:

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Abstract: (SISSA)

Recent years have brought strong observational evidences for the standard LCDM cosmologicalmodel. Cosmic microwave background (CMB) anisotropy and large scale structure (LSS) probesdo not favour any extensions of the standard model. Nevertheless, in this framework, the preferedcosmological parameters may differ from probe to probe, from experiment to experiment. This isthe well known case of the tension between CMB and Sunyaev Zel’dovich (SZ) galaxy clusters(GC) from Planck. In 2013, the Planck team has shown that the prefered matter content (WM)and density fluctuation power spectrum amplitude (s8), the two main cosmological parametersprobed by the galaxy cluster number count, are different in the CMB analyses and in the SZcluster analyses at more than 2 sigmas (a result confirmed in subsequent analyses). We presentthe results of our new analysis using more recent measurements of the CMB, SZ clusters and SZpower spectrum of 2016 and show that the tension on (WM,s8) is mostly releaved. The lowervalue of the reionisation optical depth and thus of s8 in the recent Planck studies is the mainreason. We also show that basic extensions of the standard model (massive neutrinos or non–lambda dark energy) do not help improving the agreement between the probes. In order to fullyreconcile SZ clusters with CMB best model, the mass of the galaxy clusters should be 40% lowerthan derived from hydrostatic equilibrium estimates. While current numerical simulations andweak lensing measurements agree for a mass bias of 20%, investigations are still going on toexplain such disagreement on the mass bias. We show that considering a mass bias evolving withredshift or mass does not help in eliminating the discrepancy.

galaxy: cluster
galaxy: cluster: mass
fluctuation: power spectrum
density: fluctuation
neutrino: massive
cosmic background radiation
satellite: Planck
structure
formation
numerical calculations

References(12)

Figures(0)

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