CONSTRAINING THE DARK ENERGY EQUATION OF STATE WITH COSMIC VOIDS

@article{Lee2009CONSTRAININGTD,
  title={CONSTRAINING THE DARK ENERGY EQUATION OF STATE WITH COSMIC VOIDS},
  author={Jounghun Lee and Daeseong Park},
  journal={The Astrophysical Journal},
  year={2009},
  volume={696},
  pages={L10 - L12}
}
Our universe is observed to be accelerating due to the dominant dark energy with negative pressure. The dark energy equation of state (w) holds a key to understanding the ultimate fate of the universe. The cosmic voids behave like bubbles in the universe so that its shapes must be quite sensitive to the background cosmology. Assuming a flat universe and using the priors on the matter density parameter (Ωm) and the dimensionless Hubble parameter (h), we demonstrate analytically that the… 

Dark Matter–Dark Energy Interaction and the Shape of Cosmic Voids

Interaction between dark matter (DM) and dark energy (DE) is one of the not completely solved problems in cosmology that has been studied extensively. This interaction affects cosmic structures. In

Effects of dark matter pressure on the ellipticity of cosmic voids

  • Z. Rezaei
  • Physics
    Monthly Notices of the Royal Astronomical Society
  • 2019
The dark matter in or around the cosmic voids affects their shapes. The thermodynamical properties of dark matter can alter the ellipticity of cosmic voids. Here, applying the dark matter equation of

Voids as a precision probe of dark energy

The shapes of cosmic voids, as measured in spectroscopic galaxy redshift surveys, constitute a promising new probe of dark energy (DE). We forecast constraints on the DE equation of state and its

Dark energy two decades after: observables, probes, consistency tests

In this review, the developments that led to the discovery of dark energy are summarized and the parametric descriptions ofdark energy and the cosmological tests that allow us to better understand its nature are discussed.

The void size function in dynamical dark energy cosmologies

We test a theoretical description of the void size distribution function against direct estimates from halo catalogues of the DEMNUni suite of large cosmological simulations. Besides standard ΛCDM,

Effect of dark energy perturbation on cosmic voids formation

In this paper, we present the effects of dark energy perturbation on the formation and abundance of cosmic voids. We consider dark energy to be a fluid with a negative pressure characterised by a

Non-comoving baryons and cold dark matter in cosmic voids

We examine the fully relativistic evolution of cosmic voids constituted by baryons and cold dark matter (CDM), represented by two non-comoving dust sources in a $$\varLambda $$ΛCDM background. For

Voids in massive neutrino cosmologies

Cosmic voids are a promising environment to characterize neutrino-induced effects on the large-scale distribution of matter in the universe. We perform a comprehensive numerical study of the

The darkness that shaped the void: dark energy and cosmic voids

We assess the sensitivity of void shapes to the nature of dark energy that was pointed out in recent studies and also investigate whether or not void shapes are useable as an observational probe in

Void halo mass function: A promising probe of neutrino mass

Cosmic voids, the underdense regions in the universe, are particularly sensitive to diffuse density components such as cosmic neutrinos. This sensitivity is enhanced by the match between void sizes
...

References

SHOWING 1-10 OF 32 REFERENCES

Probing Dark Energy Using Baryonic Oscillations in the Galaxy Power Spectrum as a Cosmological Ruler

We show that the baryonic oscillations expected in the galaxy power spectrum may be used as a "standard cosmological ruler" to facilitate accurate measurement of the cosmological equation of state.

New dark energy constraints from supernovae, microwave background, and galaxy clustering.

Using supernova, cosmic microwave background, and galaxy clustering data, we make the most accurate measurements to date of the dark energy density rho(X) as a function of cosmic time, constraining

Cosmological imprint of an energy component with general equation of state

We examine the possibility that a significant component of the energy density of the Universe has an equation of state different from that of matter, radiation, or cosmological constant ({Lambda} ).

Alternative high-z cosmic tracers and the dark energy equation of state

We propose to use alternative cosmic tracers to measure the dark energy equation of state and the matter content of the Universe [w(z) & Ωm]. Our proposed method consists of two components: (a)

Void ellipticity distribution as a probe of cosmology.

A completely analytic model for the void ellipticity distribution from physical principles, using the spatial distribution of galaxies in a void as a measure of its shape, tracking the trajectory of the void galaxies under the influence of the tidal field using Lagrangian perturbation theory.

A test of the nature of cosmic acceleration using galaxy redshift distortions

Using a new survey of more than 10,000 faint galaxies, the anisotropy parameter β = 0.70 ± 0.26 is measured, which is consistent with the standard cosmological-constant model with low matter density and flat geometry, although the error bars are still too large to distinguish among alternative origins for the accelerated expansion.

ACCELERATING UNIVERSES WITH SCALING DARK MATTER

Friedmann–Robertson–Walker universes with a presently large fraction of the energy density stored in an X-component with wX<-1/3, are considered. We find all the critical points of the system for

Weak lensing and dark energy

We study the power of upcoming weak lensing surveys to probe dark energy. Dark energy modifies the distance-redshift relation as well as the matter power spectrum, both of which affect the weak

Constraining dark energy with Sunyaev-Zel'dovich cluster surveys.

We discuss the prospects of constraining the properties of a dark energy component, with particular reference to a time varying equation of state, using future cluster surveys selected by their

Cluster Formation Rate in Models with Dark Energy

Based on flat Friedmann-Robertson-Walker cold dark matter (CDM) models driven by nonrelativistic matter and an exotic fluid (quintessence) with an equation of state pQ = wρQ (-1 ≤ w < 0), we