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

Yamamoto, Kazuhiro, Parkinson, David, Hamana, Takashi, Nichol, Robert C. and Suto, Yasushi (2007) Optimizing future imaging survey of galaxies to confront dark energy and modified gravity models. Physical Review D, 76 2: 1-10. doi:10.1103/PhysRevD.76.023504

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Author Yamamoto, Kazuhiro
Parkinson, David
Hamana, Takashi
Nichol, Robert C.
Suto, Yasushi
Title Optimizing future imaging survey of galaxies to confront dark energy and modified gravity models
Journal name Physical Review D   Check publisher's open access policy
ISSN 1550-7998
1089-4918
Publication date 2007-07
Sub-type Article (original research)
DOI 10.1103/PhysRevD.76.023504
Open Access Status File (Publisher version)
Volume 76
Issue 2
Start page 1
End page 10
Total pages 10
Place of publication College Park, MD, United States
Publisher American Physical Society
Language eng
Formatted abstract
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 weaklensing 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 ~ 10 min ; 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.
Q-Index Code C1
Q-Index Status Provisional Code
Institutional Status Non-UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
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Created: Mon, 28 Feb 2011, 09:47:35 EST