Optimizing future imaging survey of galaxies to confront dark energy and modified gravity models

Kazuhiro Yamamoto, David Parkinson, Takashi Hamana, Robert C. Nichol, Yasushi Suto

研究成果: Contribution to journalArticle査読

26 被引用数 (Scopus)

抄録

We consider the extent to which future imaging surveys of galaxies can distinguish between dark energy and modified gravity models for the origin of the cosmic acceleration. Dynamical dark energy models may have similar expansion rates as models of modified gravity, yet predict different growth of structure histories. We parametrize the cosmic expansion by the two parameters, w0 and wa, and the linear growth rate of density fluctuations by Linder's γ, independently. Dark energy models generically predict γ≈0.55, while the Dvali-Gabadadze-Porrati (DGP) model γ≈0.68. To determine if future imaging surveys can constrain γ within 20% (or Δγ<0.1), we perform the Fisher matrix analysis for a weak-lensing survey such as the ongoing Hyper Suprime-Cam (HSC) project. Under the condition that the total observation time is fixed, we compute the figure of merit (FoM) as a function of the exposure time texp. We find that the tomography technique effectively improves the FoM, which has a broad peak around texp several∼10min; a shallow and wide survey is preferred to constrain the γ parameter. While Δγ<0.1 cannot be achieved by the HSC weak-lensing survey alone, one can improve the constraints by combining with a follow-up spectroscopic survey like Wide-field Fiber-fed Multi-Object Spectrograph (WFMOS) and/or future cosmic microwave background (CMB) observations.

本文言語英語
論文番号023504
ジャーナルPhysical Review D - Particles, Fields, Gravitation and Cosmology
76
2
DOI
出版ステータス出版済み - 7 9 2007
外部発表はい

All Science Journal Classification (ASJC) codes

  • 核物理学および高エネルギー物理学
  • 物理学および天文学(その他)

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