Abstract
In this talk I focus on how the modelling of the mass-observable relation and the halo mass function can impact the accuracy and precision of cosmological constraints inferred from galaxy clusters. I present a new analysis of clusters detected in mm wavelengths by the Planck satellite, highlighting the need of an improved description and calibration for the mass-observable relation. I also discuss how to improve our analysis in view of future cluster surveys, with a particular focus on the impact of the halo mass function calibration and the need for a universal definition.
Highlights
Galaxy clusters are the largest, gravitationally bound structures in the Universe
In this talk I focus on how the modelling of the mass-observable relation and the halo mass function can impact the accuracy and precision of cosmological constraints inferred from galaxy clusters
We focus on how different modelling and assumptions for scaling relations and mass function can largely impact the constraints on cosmological parameters inferred from cluster number counts
Summary
Galaxy clusters are the largest, gravitationally bound structures in the Universe. They are associated with peaks in the matter density field on megaparsec scales. We rely on observables that act as massproxies and that tightly correlate with the underlying cluster mass, via some statistical scaling relation. The calibration of the scaling relations represents the current limiting systematic in cluster cosmology studies and it is usually referred to as the “masscalibration problem". In this analysis, we consider at first clusters detected in the mm-wavelengths, through the thermal Sunyaev-Zeldovich (tSZ) effect [2], by the Planck satellite [3, 4]. We focus on how different modelling and assumptions for scaling relations and mass function can largely impact the constraints on cosmological parameters inferred from cluster number counts. We comment on how these differences affect the possible tension with other cosmological probe, e.g. the σ8 discrepancy between tSZ clusters and cosmic microwave background (CMB) primary anisotropies
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