Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-26T19:27:30.689Z Has data issue: false hasContentIssue false
  • English
  • Français

Distinguishing f(R) gravity with cosmic voids

Published online by Cambridge University Press:  12 October 2016

P. Zivick  and
P. M. Sutter
P. Zivick*
Affiliation:
Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, USA
P. M. Sutter
Affiliation:
Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, USA Sorbonne Universités, UPMC Univ Paris 06, UMR7095, F-75014, Paris, France CNRS, UMR7095, Institut d'Astrophysique de Paris, F-75014, Paris, France
*
1email: zivick.1@osu.edu
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We use properties of void populations identified in N-body simulations to forecast the ability of upcoming galaxy surveys to differentiate models of f(R) gravity from \lcdm cosmology. We analyze simulations designed to mimic the densities, volumes, and clustering statistics of upcoming surveys, using the public {\tt VIDE} toolkit. We examine void abundances as a basic probe at redshifts 1.0 and 0.4. We find that stronger f(R) coupling strengths produce voids up to ∼20% larger in radius, leading to a significant shift in the void number function. As an initial estimate of the constraining power of voids, we use this change in the number function to forecast a constraint on the coupling strength of Δ fR0 = 10-5.

Keywords

cosmology: simulationscosmology: large-scale structure of universe
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 589 - 590
Copyright
Copyright © International Astronomical Union 2016 

References

Khoury, J. & Weltman, A., 2004, Phys. Rev. D, 69 Google Scholar
Laureijs, R., Amiaux, J., Arduini, S., Auguères, J., Brinchmann, J., Cole, R., Cropper, M., Dabin, C., Duvet, L., & Ealet, A., et al., 2011, ArXiv:1110.3193Google Scholar
Li, B., Zhao, G.-B., & Koyama, K., 2012, MNRAS, 421, 3481 CrossRefGoogle Scholar
Neyrinck, M. C., 2008, MNRAS, 386, 2101 CrossRefGoogle Scholar
Sutter, P. M., Carlesi, E., Wandelt, B. D., & Knebe, A., 2014, ArXiv e-printsGoogle Scholar
Sutter, P. M., et al., 2014, ArXiv e-prints: 1406.1191Google Scholar
Sutter, P. M., Lavaux, G., Wandelt, B. D., Hamaus, N., Weinberg, D. H., & Warren, M. S., 2013, ArXiv e-prints: 1309.5087Google Scholar
Zhao, B., Li, B., & Koyama, K., 2011, Phys. Rev. D, 83 Google Scholar