Simultaneous effect of Modified Gravity and Primordial Non-Gaussianity in Large Scale Structure Observations

Abstract

In this work we study the simultaneous effect of primordial non-Gaussianity and the modification of the gravity in $f(R)$ framework on large scale structure observations. We show that non-Gaussianity and modified gravity introduce a scale dependent bias and growth rate functions. The deviation from $\Lambda$CDM in the case of primordial non-Gaussian models is in large scales, while the growth rate deviates from $\Lambda$CDM in small scales for modified gravity theories. We show that the redshift space distortion can be used to distinguish positive and negative $f_{NL}$ in standard background, while in $f(R)$ theories they are not easily distinguishable. The galaxy power spectrum is generally enhanced in presence of non-Gaussianity and modified gravity. We also obtain the scale dependence of this enhancement. Finally we define galaxy growth rate and galaxy growth rate bias as new observational parameters to constrain cosmology.

18 pages, 10 figures, published in JCAP, Final Version

References in corpus (32)

• Models of f(R) Cosmic Acceleration that Evade Solar-System Tests
• Improved Cosmological Constraints from New, Old and Combined Supernova Datasets
• Cosmological Constraints from the SDSS Luminous Red Galaxies
• Disappearing cosmological constant in f(R) gravity
• The imprints of primordial non-gaussianities on large-scale structure: scale dependent bias and abundance of virialized objects
• Palatini Approach to Modified Gravity: f(R) Theories and Beyond
• A test of the nature of cosmic acceleration using galaxy redshift distortions
• The Large Scale Structure of f(R) Gravity
• A Parameterized Post-Friedmann Framework for Modified Gravity
• Confirmation of general relativity on large scales from weak lensing and galaxy velocities
• Distinguishing Modified Gravity from Dark Energy
• Effects of Scale-Dependent Non-Gaussianity on Cosmological Structures
• Solar System tests DO rule out 1/R gravity
• The 2dF-SDSS LRG and QSO Survey: QSO clustering and the L-z degeneracy
• The 2dF-SDSS LRG and QSO Survey: The LRG 2-Point Correlation Function and Redshift-Space Distortions
• Primordial non-gaussianity, statistics of collapsed objects, and the Integrated Sachs-Wolfe effect
• A Hemispherical Power Asymmetry from Inflation
• Constraints on scalar-tensor models of dark energy from observational and local gravity tests
• Superhorizon Perturbations and the Cosmic Microwave Background
• Primordial non-Gaussianity, scale-dependent bias, and the bispectrum of galaxies
• The dispersion of growth of matter perturbations in f(R) gravity
• Primordial non-Gaussianity in the large scale structure of the Universe
• Modified gravity with $f(R)=\sqrt{R^2-R_0^2}$
• Cosmic tomographies: baryon acoustic oscillations and weak lensing
• Consistency of $f(R)=\sqrt{R^2-R_0^2}$ Gravity with the Cosmological Observations in Palatini Formalism
• Hemispherical Asymmetry and Local non-Gaussianity: a Consistency Condition
• Scale-dependent halo bias from scale-dependent growth
• Parametrized modified gravity constraints after Planck
• Cosmological constraints on the Hu-Sawicki modified gravity scenario
• Parametrised modified gravity and the CMB Bispectrum
• Observational tests of a two parameter power-law class modified gravity in Palatini formalism
• Structure formation in $f(R)$ gravity: A distinguishing probe between the dark energy and modified gravity

Cited by in corpus (9)

• Constraining chameleon models with cosmology
• An Accurate Fitting Function For Scale-dependent Growth Rate in Hu-Sawicki $f(R)$ Gravity
• Late time sky as a probe of steps and oscillations in primordial Universe
• Probing gravity with redshift-space distortions: effects of tracer bias and sample selection
• ISW-Galaxy Cross Correlation:A probe of Dark Energy clustering and distribution of Dark Matter tracers
• Perturbation level interacting dark energy model and its consequence on late-time cosmological parameters
• Unraveling the nature of Gravity through our clumpy Universe
• Testing time-delayed cosmology
• Scalar perturbation and density contrast evolution in $f(Q,C)$ gravity