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ORIGINAL RESEARCH article

Front. Astron. Space Sci.
Sec. Astronomical Instrumentation
Volume 11 - 2024 | doi: 10.3389/fspas.2024.1411810
This article is part of the Research Topic New Telescope Advances with Novel Techniques View all 10 articles

Measurement and Calibration of Non-Linear Shear Terms in Galaxy Cluster Fields

Provisionally accepted
Binyang Liu Binyang Liu 1,2*Ian Dell'antonio Ian Dell'antonio 1*Nicolas Chotard Nicolas Chotard 3*Douglas Clowe Douglas Clowe 4*
  • 1 Brown University, Providence, Rhode Island, United States
  • 2 Purple Mountain Observatory, Chinese Academy of Sciences (CAS), Nanjing, China
  • 3 Institut National de Physique NuclΓ©aire et de Physique des Particules (CNRS), Paris, Île-de-France, France
  • 4 Ohio University, Athens, West Virginia, United States

The final, formatted version of the article will be published soon.

    Introduction: Galaxy cluster lensing is a powerful tool for measuring the mass of galaxy clusters, but accurate shear measurement and calibration are critical to obtaining reliable results. This study focuses on the measurement and calibration of weak lensing shears to improve mass estimates in cluster lensing. To deal with the problem, we first developed an image simulation pipeline, jedisim, which utilizes galaxy images extracted from the Hubble Space Telescope (HST) Ultra Deep Field (UDF) and the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS).The simulations represent realistic galaxy distributions and morphologies as input sources.The foreground halo with NFW profile is constructed such that the lensing signals of background galaxies can be measured by the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST) Science Pipelines. By comparing the measured reduced shear 𝑔 meas and the true reduced shear 𝑔 true , we observe non-linearity up to 𝑔 ≲ 0.6. We fit polynomials to the data with quadratic correction adequate to 𝑔 ≲ 0.4. In the meantime, we conduct mass estimate with the pzmassfitter code on 4 different clusters.The mass estimate results are significantly improved after applying the shear calibration derived from the present work -from 4.954Β±0.504Γ—10 14 𝑀 βŠ™ to 10.507Β±0.498Γ—10 14 𝑀 βŠ™ after calibration for a simulated cluster with the mass of 10 Γ— 10 14 𝑀 βŠ™ . In multiple cases of validations, the estimated results are all consistent with true cluster mass.Discussion: This study yields a first relationship between reality and shape measurement of the LSST Science Pipelines and serves as the first step of the overall goal of mass calibration in cluster lensing.By addressing the challenges in shear measurement and calibration, we aim to enhance the accuracy and reliability of mass estimates in galaxy cluster lensing studies.

    Keywords: galaxy clusters, gravitational lensing, image processing, Observational cosmology, Systematic uncertainties

    Received: 03 Apr 2024; Accepted: 08 Jul 2024.

    Copyright: Β© 2024 Liu, Dell'antonio, Chotard and Clowe. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) or licensor are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

    * Correspondence:
    Binyang Liu, Brown University, Providence, 02912, Rhode Island, United States
    Ian Dell'antonio, Brown University, Providence, 02912, Rhode Island, United States
    Nicolas Chotard, Institut National de Physique Nucléaire et de Physique des Particules (CNRS), Paris, 75794, Île-de-France, France
    Douglas Clowe, Ohio University, Athens, 45701, West Virginia, United States

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