scholarly journals Cosmological Surveys with the Australian Square Kilometre Array Pathfinder

2012 ◽  
Vol 29 (2) ◽  
pp. 202-211 ◽  
Author(s):  
A. R. Duffy ◽  
A. Moss ◽  
L. Staveley-Smith
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Power Spectrum ◽  
Energy Equation ◽  
Coming Of Age ◽  
Neutral Hydrogen ◽  
Square Kilometre Array ◽  
Cosmological Constraints ◽  
Sky Survey ◽  
The Galaxy

AbstractThis is a design study into the capabilities of the Australian Square Kilometre Array Pathfinder in performing a full-sky low redshift neutral hydrogen survey, termed WALLABY, and the potential cosmological constraints one can attain from measurement of the galaxy power spectrum. We find that the full sky survey will likely attain 6 × 105 redshifts which, when combined with expected Planck CMB data, will constrain the Dark Energy equation of state to 20%, representing a coming of age for radio observations in creating cosmological constraints.

scholarly journals MEASURING NEUTRINO MASSES AND DARK ENERGY

2008 ◽  
Vol 23 (34) ◽  
pp. 2881-2895
Author(s):  
HUITZU TU
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Neutrino Mass ◽  
Energy Equation ◽  
Mass Scale ◽  
Neutrino Masses ◽  
Acoustic Oscillations ◽  
Distance Measurements ◽  
The Galaxy ◽  
Absolute Neutrino Mass

We review some recent efforts in determining the absolute neutrino mass scale in cosmology. We illustrate in particular how distance measurements such as the baryon acoustic oscillations and the galaxy weak lensing can break the degeneracy between the neutrino mass and dark energy equation of state parameters.

scholarly journals Constraints on the dark energy equation of state from the imprint of baryons on the power spectrum of clusters

2005 ◽  
Vol 362 (1) ◽  
pp. L25-L29 ◽  
Author(s):  
R. Angulo ◽  
C. M. Baugh ◽  
C. S. Frenk ◽  
R. G. Bower ◽  
A. Jenkins ◽  
...  
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Power Spectrum ◽  
Energy Equation

CONSTRAINTS ON THE DARK ENERGY EQUATION OF STATE IN PRESENCE OF A VARYING FINE STRUCTURE CONSTANT

2010 ◽  
Vol 19 (04) ◽  
pp. 507-512 ◽  
Author(s):  
E. MENEGONI ◽  
S. PANDOLFI ◽  
S. GALLI ◽  
M. LATTANZI ◽  
A. MELCHIORRI
Keyword(s):  
Fine Structure ◽  
Dark Energy ◽  
Equation Of State ◽  
Cosmological Constant ◽  
Energy Equation ◽  
Structure Constant ◽  
Hubble Constant ◽  
Fine Structure Constant ◽  
Cosmological Constraints ◽  
Energy Models

We discuss the cosmological constraints on the dark energy equation of state in the presence of primordial variations in the fine structure constant. We find that the constraints from CMB data alone on w and the Hubble constant are much weaker when variations in the fine structure constant are permitted. Vice versa, constraints on the fine structure constant are relaxed by more than 50% when dark energy models different from a cosmological constant are considered.

scholarly journals Measuring the Hubble function with standard candle clustering

2021 ◽  
Author(s):  
Luca Amendola ◽  
Miguel Quartin
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Power Spectrum ◽  
Energy Equation ◽  
Luminosity Distance ◽  
Distortion Parameter ◽  
Peculiar Velocities ◽  
Matter Power Spectrum ◽  
Standard Candle ◽  
Model Independent

Abstract Supernova Ia magnitude surveys measure the dimensionless luminosity distance H0DL. However, from the distances alone one cannot obtain quantities like H(z) or the dark energy equation of state, unless further cosmological assumptions are imposed. Here we show that by measuring the power spectrum of density contrast and of peculiar velocities of supernovae one can estimate also H(z)/H0 regardless of background or linearly perturbed cosmology and of galaxy-matter bias. This method, dubbed Clustering of Standard Candles (CSC) also yields the redshift distortion parameter β(k, z) and the biased matter power spectrum in a model-independent way. We forecast that an optimistic (pessimistic) LSST may be able to constrain H(z)/H0 to 5–13% (9–40%) in redshift bins of Δz = 0.1 up to at least z = 0.6.

scholarly journals Nonparametric reconstruction of the dark energy equation of state from diverse data sets

2011 ◽  
Vol 84 (8) ◽  
Author(s):  
Tracy Holsclaw ◽  
Ujjaini Alam ◽  
Bruno Sansó ◽  
Herbie Lee ◽  
Katrin Heitmann ◽  
...  
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Energy Equation ◽  
Data Sets ◽  
Diverse Data

scholarly journals Impact of relativistic effects on the primordial non-Gaussianity signature in the large-scale clustering of quasars

2020 ◽  
Vol 499 (2) ◽  
pp. 2598-2607
Author(s):  
Mike (Shengbo) Wang ◽  
Florian Beutler ◽  
David Bacon
Keyword(s):  
Dark Energy ◽  
Power Spectrum ◽  
Luminosity Function ◽  
Large Scale ◽  
Relativistic Effects ◽  
Redshift Range ◽  
Cosmological Background ◽  
Relativistic Corrections ◽  
The Galaxy ◽  
The Impact

ABSTRACT Relativistic effects in clustering observations have been shown to introduce scale-dependent corrections to the galaxy overdensity field on large scales, which may hamper the detection of primordial non-Gaussianity fNL through the scale-dependent halo bias. The amplitude of relativistic corrections depends not only on the cosmological background expansion, but also on the redshift evolution and sensitivity to the luminosity threshold of the tracer population being examined, as parametrized by the evolution bias be and magnification bias s. In this work, we propagate luminosity function measurements from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) to be and s for the quasar (QSO) sample, and thereby derive constraints on relativistic corrections to its power spectrum multipoles. Although one could mitigate the impact on the fNL signature by adjusting the redshift range or the luminosity threshold of the tracer sample being considered, we suggest that, for future surveys probing large cosmic volumes, relativistic corrections should be forward modelled from the tracer luminosity function including its uncertainties. This will be important to quasar clustering measurements on scales $k \sim 10^{-3}\, h\, {\rm Mpc}^{-1}$ in upcoming surveys such as the Dark Energy Spectroscopic Instrument (DESI), where relativistic corrections can overwhelm the expected fNL signature at low redshifts z ≲ 1 and become comparable to fNL ≃ 1 in the power spectrum quadrupole at redshifts z ≳ 2.5.

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