Cosmic growth history and expansion history

By Eric Linder. 2005

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Author(s): Linder, Eric V. | Abstract: The cosmic expansion history tests the dynamics of the global evolution of the universe and its energy density contents, while the cosmic growth history tests the evolution of the inhomogeneous part of the energy density. Precision comparison of the two histories can distinguish the nature of the physics responsible for the accelerating cosmic expansion: an additional smooth component - dark energy - or a modification of the gravitational field equations. With the aid of a new fitting formula for linear perturbation growth accurate to 0.05-0.2percent, we separate out the growth dependence on the expansion history and introduce a new growth index parameter \gamma that quantifies the gravitational modification.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d266d6c34ee9c01c0a78150e6abb320a9d1d01c3

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Citations in the corpus

THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGY FROM GALAXY CLUSTERS DETECTED VIA THE SUNYAEV–ZEL'DOVICH EFFECT (2010, background): “A deviation from this predicted growth rate, particularly on linear scales, would signal a breakdown of ΛCDM (see, e.g., Linder 2005; Bertschinger & Zukin 2008; Silvestri & Trodden 2009; Jain & Khoury 2010; Shapiro et al. 2010, and references therein).”
The 6dF Galaxy Survey: z \approx 0 measurement of the growth rate and sigma_8 (2012, background): “Because of the missing dark energy component, this model predicts a larger growth index of γ ≈ 0.69 (Linder 2005).”
Observational probes of cosmic acceleration (2012, background): “Some choices give a nearly constant w that is different from −1, while others have w ≈ −1 as an asymptotic state at either early or late times, referred to respectively as “thawing” or “freezing” solutions (Caldwell and Linder, 2005).”
Cosmological Parameters from Observations of Galaxy Clusters (2011, background): “At late-times, the linear growth rate can be simply parametrized as (e.g. Linder 2005) d ln δ d ln a = Ωm(a) γ , (26) where δ is the density contrast and γ the growth index.”
Brane-World Gravity (2004, neutral): “If we parametrize the growth factor in the usual way, we can quantify the deviation from general relativity with smooth dark energy [293]:”
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Fourier space (2016, methodology): “With this ‘standard ruler’ technique one can map the expansion history of the Universe (e.g. Hu & White 1996; Blake & Astrophys 2003; Eisenstein 2003; Hu & Haiman 2003; Seo & Eisenstein 2003; Linder 2005).”
Modified Gravity and Cosmology (2011, methodology): “or by the introduction of a parameter γ through [1031, 813, 783, 784]”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “…cosmological models in different gravity theories that predict a similarexpansion rate can have different values off via a change to the Poisson equation (Wang & Steinhardt 1998; Linder 2005) and demonstrated that it is potentially possible to distinguish different theories of gravity using RSD.”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, neutral): “As usual, we use the simple prescription [938, 721, 978, 776, 1223]”
Ultrahigh precision cosmology from gravitational waves (2009, neutral): “Rev. 14 D 74, 063006 [36] S. Nissanke et al. 2009, arXiv:0904.1017 [37] Frieman, J. A. 1997, Comments Astrophys., 18, 323 [38] D. E. Holz and R. M. Wald 1998, PRD, 58, 063501 [39] D. E. Holz and E. V. Linder 2005, Astrophys.”