Euclid preparation
Astronomy and Astrophysics, vol. 695, pp. A280
Abstract
The ability to measure unbiased weak-lensing (WL) masses is a key ingredient to exploit galaxy clusters as a competitive cosmological probe with the ESA Euclid survey or future missions. We investigate the level of accuracy and precision of cluster masses measured with the Euclid data processing pipeline. We use the DEMNUni-Cov N -body simulations to assess how well the WL mass probes the true halo mass, and, then, how well WL masses can be recovered in the presence of measurement uncertainties. We consider different halo mass density models, priors, and mass point estimates, that is the biweight, mean, and median of the marginalised posterior distribution and the maximum likelihood parameter. WL mass differs from true mass due to, for example, the intrinsic ellipticity of sources, correlated or uncorrelated matter and large-scale structure, halo triaxiality and orientation, and merging or irregular morphology. In an ideal scenario without observational or measurement errors, the maximum likelihood estimator is the most accurate, with WL masses biased low by ⟨ b M ⟩= − 14.6 ± 1.7% on average over the full range M 200c > 5 × 10 13 M ⊙ and z < 1. Due to the stabilising effect of the prior, the biweight, mean, and median estimates are more precise, that is with smaller intrinsic scatter. The scatter decreases with increasing mass and informative priors can significantly reduce the scatter. Halo mass density profiles with a truncation provide better fits to the lensing signal, while the accuracy and precision are not significantly affected. We further investigate the impact of various additional sources of systematic uncertainty on the WL mass estimates, namely the impact of photometric redshift uncertainties and source selection, the expected performance of Euclid cluster detection algorithms, and the presence of masks. Taken in isolation, we find that the largest effect is induced by non-conservative source selection with ⟨ b M ⟩= − 33.4 ± 1.6%. This effect can be mostly removed with a robust selection. As a final Euclid -like test, we combine systematic effects in a realistic observational setting and find ⟨ b M ⟩= − 15.5 ± 2.4% under a robust selection. This is very similar to the ideal case, though with a slightly larger scatter mostly due to cluster redshift uncertainty and miscentering.
Authors 21
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Istituto di Radioastronomia di Bologna · National Institute for Astrophysics · University of Bologna
Affiliation as printed
Dipartimento di Fisica e Astronomia “Augusto Righi” – Alma Mater Studiorum Università di Bologna
INAF, Istituto di Radioastronomia
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Istituto Nazionale di Fisica Nucleare, Sezione di Bologna · Osservatorio di Astrofisica e Scienza dello Spazio · National Institute for Astrophysics
Affiliation as printed
INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna
INFN-Sezione di Bologna
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Centre National de la Recherche Scientifique · Université Paris Cité · Commissariat à l'Énergie Atomique et aux Énergies Alternatives · Université Paris-Saclay · Astrophysique, Instrumentation et Modélisation
Affiliation as printed
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM
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Istituto Nazionale di Fisica Nucleare, Sezione di Bologna · Osservatorio di Astrofisica e Scienza dello Spazio · National Institute for Astrophysics
Affiliation as printed
INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna
Istituto Nazionale di Fisica Nucleare, Sezione di Bologna
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Centre National de la Recherche Scientifique · Université Paris Cité · Commissariat à l'Énergie Atomique et aux Énergies Alternatives · Université Paris-Saclay · Astrophysique, Instrumentation et Modélisation
Affiliation as printed
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM
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Istituto Nazionale di Fisica Nucleare, Sezione di Bologna · Osservatorio di Astrofisica e Scienza dello Spazio · National Institute for Astrophysics · University of Bologna
Affiliation as printed
Dipartimento di Fisica e Astronomia “Augusto Righi” – Alma Mater Studiorum Università di Bologna
INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna
INFN-Sezione di Bologna
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Trieste Astronomical Observatory · Institute for Fundamental Physics of the Universe · National Institute for Astrophysics
Affiliation as printed
IFPU, Institute for Fundamental Physics of the Universe
INAF-Osservatorio Astronomico di Trieste
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Istituto Nazionale di Fisica Nucleare, Sezione di Bologna · Osservatorio di Astrofisica e Scienza dello Spazio · National Institute for Astrophysics
Affiliation as printed
INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna
INFN-Sezione di Bologna
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Osservatorio Astronomico di Padova · National Institute for Astrophysics
Affiliation as printed
INAF-Osservatorio Astronomico di Padova
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Affiliation as printed
School of Mathematics and Physics, University of Surrey
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Centre National de la Recherche Scientifique · Commissariat à l'Énergie Atomique et aux Énergies Alternatives · Université Paris-Saclay · Institut d'Astrophysique de Paris · Sorbonne Université · Institut de Physique Théorique
Affiliation as printed
Institut de Physique Théorique, CEA, CNRS, Université Paris-Saclay
Institut d’Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université
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Osservatorio di Astrofisica e Scienza dello Spazio · National Institute for Astrophysics
Affiliation as printed
INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna
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European Space Agency · European Space Astronomy Centre
Affiliation as printed
ESAC/ESA
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Institute of Space Sciences · Institut d'Estudis Espacials de Catalunya · Universitat Politècnica de Catalunya
Affiliation as printed
Institut d’Estudis Espacials de Catalunya (IEEC), Edifici RDIT, Campus UPC
Institute of Space Sciences (ICE, CSIC), Campus UAB
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Centre National de la Recherche Scientifique · Institut d'Astrophysique de Paris · Sorbonne Université
Affiliation as printed
Institut d’Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université
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Centre National de la Recherche Scientifique · Université Toulouse III - Paul Sabatier · Université Paris-Saclay · Institut National de Physique Nucléaire et de Physique des Particules · Laboratoire de Physique des 2 Infinis Irène Joliot-Curie · Institut de Recherche en Astrophysique et Planétologie · Université de Toulouse
Affiliation as printed
Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES
Université Paris-Saclay, CNRS/IN2P3, IJCLab
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Max Planck Institute for Astronomy
Affiliation as printed
Max-Planck-Institut für Astronomie
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Centre National de la Recherche Scientifique · Aix-Marseille Université · Centre de physique des particules de Marseille · Institut National de Physique Nucléaire et de Physique des Particules
Affiliation as printed
Aix-Marseille Université, CNRS/IN2P3, CPPM
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Centre National de la Recherche Scientifique · Université Paris Cité · Commissariat à l'Énergie Atomique et aux Énergies Alternatives · Université Paris-Saclay · Astrophysique, Instrumentation et Modélisation
Affiliation as printed
Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM
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Affiliation as printed
Department of Physics
Helsinki Institute of Physics
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Centre National de la Recherche Scientifique · Aix-Marseille Université
Affiliation as printed
Aix-Marseille Université, CNRS, CNES, LAM
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