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  1. academic.oup.com

    For chameleon gravity, cluster observations provide the most stringent constraints to date on cosmological scales (mega to gigaparsec scales) and are complementary to the Solar system and dwarf galaxy tests which probe smaller scales (up to kiloparsec scales).
    Author:Harry Wilcox, Robert C. Nichol, Gong-Bo Zhao, David Bacon, Kazuya Koyama, A. Kathy RomerPublished:2016
  2. We use two new hydrodynamical simulations of CDM and gravity to test the methodology used by Wilcox et al. 2015 (W15) in constraining the effects of a fifth force on the profiles of clusters of galaxies. We construct realistic simulated stacked weak lensing and X-ray surface brightness cluster profiles from these cosmological simulations, and then use these data projected along various lines ...
  3. researchgate.net

    Simulation tests of galaxy cluster constraints on chameleon gravity March 2016 Monthly Notices of the Royal Astronomical Society 462 (1) DOI: 10.1093/mnras/stw1617 Authors: H. Wilcox
  4. cordis.europa.eu

    Simulation tests of galaxy cluster constraints on chameleon gravity Author (s): Harry Wilcox, Robert C. Nichol, Gong-Bo Zhao, David Bacon, Kazuya Koyama, A. Kathy Romer Published in: Monthly Notices of the Royal Astronomical Society, Issue 462/1, 2016, Page (s) 715-725, ISSN 0035-8711Publisher: Blackwell Publishing Inc. DOI: 10.1093/mnras/stw1617
  5. semanticscholar.org

    Figure 3. A mosaic of four (projected) cluster profiles taken from the CDM+GR simulation at z = 0.4. The coloured contours are the gas density, while the black contour lines are the gas temperature. Here, the redder contours denote higher temperatures and bluer lower over a scale of 2-0.5 keV. - "Simulation tests of galaxy cluster constraints on chameleon gravity"
  6. ieeexplore.ieee.org

    We use two new hydrodynamical simulations of Λ cold dark matter (ΛCDM) and f(R) gravity to test the methodology used by Wilcox et al. (W15) in constraining the effects of a fifth force on the profiles of clusters of galaxies. We construct realistic simulated stacked weak lensing and X-ray surface brightness cluster profiles from these cosmological simulations, and then use these data ...
  7. Abstract. The chameleon screening mechanism has been constrained many a time using dynamic and kinematic galaxy cluster observables. Current constraints are, however, insensitive to diferent mass components within galaxy clusters and have been mainly focused on a single mass density profile, the Navarro-Frenk-While mass density model.
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