scholarly journals Modelling galaxy clustering on small scales to tighten constraints on dark energy and modified gravity

2016 ◽  
Vol 464 (3) ◽  
pp. 3005-3012 ◽  
Author(s):  
Yun Wang
Keyword(s):  
Dark Energy ◽  
Modified Gravity ◽  
Galaxy Clustering ◽  
Small Scales

Editorial [Dark Energy and Modified Gravity]

2010 ◽  
Vol 3 (2) ◽  
pp. 12-12
Author(s):  
S. Nojiri ◽  
S. D. Odintsov
Keyword(s):  
Dark Energy ◽  
Modified Gravity

BOUNDS ON f(G) GRAVITY FROM ENERGY CONDITIONS

2010 ◽  
Vol 25 (27) ◽  
pp. 2325-2332 ◽  
Author(s):  
PUXUN WU ◽  
HONGWEI YU
Keyword(s):  
General Relativity ◽  
Dark Energy ◽  
Energy Density ◽  
Modified Gravity ◽  
Energy Conditions ◽  
Model Parameters ◽  
Effective Energy ◽  
Raychaudhuri Equation ◽  
Accelerating Expansion

The f(G) gravity is a theory to modify the general relativity and it can explain the present cosmic accelerating expansion without the need of dark energy. In this paper the f(G) gravity is tested with the energy conditions. Using the Raychaudhuri equation along with the requirement that the gravity is attractive in the FRW background, we obtain the bounds on f(G) from the SEC and NEC. These bounds can also be found directly from the SEC and NEC within the general relativity context by the transformations: ρ → ρm + ρE and p → pm + pE, where ρE and pE are the effective energy density and pressure in the modified gravity. With these transformations, the constraints on f(G) from the WEC and DEC are obtained. Finally, we examine two concrete examples with WEC and obtain the allowed region of model parameters.

GROWTH INDEX AND MODIFIED GRAVITY

2011 ◽  
Vol 01 ◽  
pp. 228-233
Author(s):  
YUNGUI GONG
Keyword(s):  
Growth Rate ◽  
Dark Energy ◽  
Modified Gravity ◽  
Growth Index ◽  
Accurate Approximation ◽  
Energy Models ◽  
Λcdm Model ◽  
The Universe ◽  
Matter Energy ◽  
Matter Perturbation

The growth rate of matter perturbation and the expansion rate of the Universe can be used to distinguish modified gravity and dark energy models. Remarkably, the growth rate can be approximated as Ωγ. We discuss the dependence of the growth index γ on the dimensionless matter energy density Ω for a more accurate approximation of the growth factor. The observational data are used to fit different models. The data strongly disfavor the Dvali-Gabadadze-Porrati model. For the ΛCDM model, we find that [Formula: see text]. For the Dvali-Gabadadze-Porrati model, we find that [Formula: see text].

scholarly journals On model selection forecasting, dark energy and modified gravity

2007 ◽  
Vol 380 (3) ◽  
pp. 1029-1035 ◽  
Author(s):  
A. F. Heavens ◽  
T. D. Kitching ◽  
L. Verde
Keyword(s):  
Dark Energy ◽  
Model Selection ◽  
Modified Gravity

scholarly journals Inference from the small scales of cosmic shear with current and future Dark Energy Survey data

2016 ◽  
Vol 465 (3) ◽  
pp. 2567-2583 ◽  
Author(s):  
N. MacCrann ◽  
J. Aleksić ◽  
A. Amara ◽  
S. L. Bridle ◽  
C. Bruderer ◽  
...  
Keyword(s):  
Dark Energy ◽  
Survey Data ◽  
Dark Energy Survey ◽  
Small Scales ◽  
Cosmic Shear ◽  
Energy Survey

scholarly journals Dark energy versus modified gravity: Impacts on measuring neutrino mass

2020 ◽  
Vol 63 (3) ◽  
Author(s):  
MingMing Zhao ◽  
RuiYun Guo ◽  
DongZe He ◽  
JingFei Zhang ◽  
Xin Zhang
Keyword(s):  
Dark Energy ◽  
Neutrino Mass ◽  
Modified Gravity

scholarly journals Cosmological Implications of the Generalized Entropy Based Holographic Dark Energy Models in Dynamical Chern-Simons Modified Gravity

2019 ◽  
Vol 2019 ◽  
pp. 1-9 ◽  
Author(s):  
M. Younas ◽  
Abdul Jawad ◽  
Saba Qummer ◽  
H. Moradpour ◽  
Shamaila Rani
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Modified Gravity ◽  
Dark Energy Model ◽  
State Parameter ◽  
Energy Model ◽  
Evolutionary Equation ◽  
Energy Models ◽  
Equation Of State Parameter ◽  
Chern Simons

Recently, Tsallis, Rényi, and Sharma-Mittal entropies have widely been used to study the gravitational and cosmological setups. We consider a flat FRW universe with linear interaction between dark energy and dark matter. We discuss the dark energy models using Tsallis, Rényi, and Sharma-Mittal entropies in the framework of Chern-Simons modified gravity. We explore various cosmological parameters (equation of state parameter, squared sound of speed ) and cosmological plane (ωd-ωd′, where ωd′ is the evolutionary equation of state parameter). It is observed that the equation of state parameter gives quintessence-like nature of the universe in most of the cases. Also, the squared speed of sound shows stability of Tsallis and Rényi dark energy model but unstable behavior for Sharma-Mittal dark energy model. The ωd-ωd′ plane represents the thawing region for all dark energy models.

scholarly journals Dark Energy Survey year 1 results: Joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

2019 ◽  
Vol 100 (2) ◽  
Author(s):  
T. M. C. Abbott ◽  
F. B. Abdalla ◽  
A. Alarcon ◽  
S. Allam ◽  
J. Annis ◽  
...  
Keyword(s):  
Dark Energy ◽  
Joint Analysis ◽  
Galaxy Clustering ◽  
Dark Energy Survey ◽  
Energy Survey
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