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The impact of dark energy perturbations on the growth index
Cosmology and Nongalactic Astrophysics · Submitted 12 Mar 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show that in clustering dark energy models the growth index of linear matter perturbations, $\gamma$, can be much lower than in $\Lambda$CDM or smooth quintessence models and present a strong variation with redshift.
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The abstract, sentence by sentence
We show that in clustering dark energy models the growth index of linear matter perturbations, $\gamma$, can be much lower than in $\Lambda$CDM or smooth quintessence models and present a strong variation with redshift. We find that the impact of dark energy perturbations on $\gamma$ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have $0.33<\gamma\left(z\right)<0.48$ at $0<z<3$. We also show that the constant $\gamma$ parametrization for the growth rate, $f=d\ln\delta_{m}/d\ln a=\Omega_{m}^{\gamma}$, is a few percent inaccurate for such models and that a redshift dependent parametrization for $\gamma$ can provide about four times more accurate fits for $f$. We discuss the robustness of the growth index to distinguish between General Relativity with clustering dark energy and modified gravity models, finding that some $f\left(R\right)$ and clustering dark energy models can present similar values for $\gamma$.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We show that in clustering dark energy models the growth index of linear matter perturbations, $\gamma$, can be much lower than in $\Lambda$CDM or smooth quintessence models and present a strong variation with redshift. | result 0.94 | 0.94 | 0.79 | asserted 1.00 |
| s1 | We find that the impact of dark energy perturbations on $\gamma$ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. | result 0.99 | 0.94 | 0.14 | asserted 1.00 |
| s2 | We study four different models with these features and show that we may have $0.33<\gamma\left(z\right)<0.48$ at $0<z<3$. | result 0.97 | 0.96 | 0.23 | hedged possibility 0.88 |
| s3 | We also show that the constant $\gamma$ parametrization for the growth rate, $f=d\ln\delta_{m}/d\ln a=\Omega_{m}^{\gamma}$, is a few percent inaccurate for such models and that a redshift dependent parametrization for $\gamma$ can provide about four times more accurate fits for $f$. | result 0.98 | 0.93 | 0.13 | asserted 1.00 |
| s4 | We discuss the robustness of the growth index to distinguish between General Relativity with clustering dark energy and modified gravity models, finding that some $f\left(R\right)$ and clustering dark energy models can present similar values for $\gamma$. | interpretation 0.46 | 0.88 | 0.09 | hedged possibility 0.73 |
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Original abstract
We show that in clustering dark energy models the growth index of linear matter perturbations, $\gamma$, can be much lower than in $\Lambda$CDM or smooth quintessence models and present a strong variation with redshift. We find that the impact of dark energy perturbations on $\gamma$ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have $0.33<\gamma\left(z\right)<0.48$ at $0<z<3$. We also show that the constant $\gamma$ parametrization for the growth rate, $f=d\ln\delta_{m}/d\ln a=\Omega_{m}^{\gamma}$, is a few percent inaccurate for such models and that a redshift dependent parametrization for $\gamma$ can provide about four times more accurate fits for $f$. We discuss the robustness of the growth index to distinguish between General Relativity with clustering dark energy and modified gravity models, finding that some $f\left(R\right)$ and clustering dark energy models can present similar values for $\gamma$.
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7 arXiv papers cite this in 11 sentences
Papers citing it · 8 sentences without a confident label
Compares with it 1 paper
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The results found here from our analytic formula are in very good agreement with those that can be found in the literature, see for example [ref] .
Sub-horizon evolution of cold dark matter perturbations through dark matter-dark energy equivalence epoch · Growth function, logarithmic growth function and growth index · 0.99
Cites it as background 2 papers
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We refer to this scenario as Clustering DE (CDE), which growth index has already been studied in [ref] .
Can dark energy explain a high growth index? · Introduction · 0.96
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In the perturbative level, there are effects on the formation of large-scale structures of the Universe which are based on the DE, e.g. the dynamical DE models [ref] .
Cosmological perturbations in the Tsallis holographic dark energy scenarios · Introduction · 0.85
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