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  Calibration of bias and scatter involved in cluster mass measurements using optical weak gravitational lensing

Grandis, S., Bocquet, S., Mohr, J. J., Klein, M., & Dolag, K. (2021). Calibration of bias and scatter involved in cluster mass measurements using optical weak gravitational lensing. Monthly Notices of the Royal Astronomical Society, 507(4), 5671-5689. doi:10.1093/mnras/stab2414.

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 Creators:
Grandis, Sebastian, Author
Bocquet, Sebastian, Author
Mohr, Joseph J.1, Author              
Klein, Matthias2, Author              
Dolag, Klaus, Author
Affiliations:
1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              
2High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society, ou_159890              

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 Abstract: Cosmological inference from cluster number counts is systematically limited by the accuracy of the mass calibration, i.e. the empirical determination of the mapping between cluster selection observables and halo mass. In this work we demonstrate a method to quantitatively determine the bias and uncertainties in weak-lensing (WL) mass calibration. To this end, we extract a library of projected matter density profiles from hydrodynamical simulations. Accounting for shear bias and noise, photometric redshift uncertainties, mis-centreing, cluster member contamination, cluster morphological diversity, and line-of-sight projections, we produce a library of shear profiles. Fitting a one-parameter model to these profiles, we extract the so-called WL mass MWL. Relating the WL mass to the halo mass from gravity-only simulations with the same initial conditions as the hydrodynamical simulations allows us to estimate the impact of hydrodynamical effects on cluster number counts experiments. Creating new shear libraries for ∼1000 different realizations of the systematics provides a distribution of the parameters of the WL to halo mass relation, reflecting their systematic uncertainty. This result can be used as a prior for cosmological inference. We also discuss the impact of the inner fitting radius on the accuracy, and determine the outer fitting radius necessary to exclude the signal from neighbouring structures. Our method is currently being applied to different Stage III lensing surveys, and can easily be extended to Stage IV lensing surveys.

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Language(s): eng - English
 Dates: 2021-09-07
 Publication Status: Published online
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 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/stab2414
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Title: Monthly Notices of the Royal Astronomical Society
  Abbreviation : Mon. Not. Roy. Astron. Soc.
Source Genre: Journal
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Pages: - Volume / Issue: 507 (4) Sequence Number: - Start / End Page: 5671 - 5689 Identifier: ISSN: 0035-8711
ISSN: 1365-8711