scholarly journals Constraints on dark energy from the Lyα forest baryon acoustic oscillations measurement of the redshift 2.3 Hubble parameter

2013 ◽  
Vol 723 (1-3) ◽  
pp. 1-6 ◽  
Author(s):  
Omer Farooq ◽  
Bharat Ratra
Keyword(s):  
Dark Energy ◽  
Hubble Parameter ◽  
Acoustic Oscillations ◽  
Baryon Acoustic Oscillations

scholarly journals What do we really know about dark energy?

2011 ◽  
Vol 369 (1957) ◽  
pp. 5102-5114 ◽  
Author(s):  
Ruth Durrer
Keyword(s):  
Dark Energy ◽  
Cosmic Microwave Background ◽  
Hubble Parameter ◽  
Acoustic Oscillations ◽  
Microwave Background ◽  
Distance Measurements ◽  
Baryon Acoustic Oscillations ◽  
The One ◽  
Microwave Background Anisotropies

In this paper, we discuss what we truly know about dark energy. I shall argue that, to date, our single indication for the existence of dark energy comes from distance measurements and their relation to redshift. Supernovae, cosmic microwave background anisotropies and observations of baryon acoustic oscillations simply tell us that the observed distance to a given redshift z is larger than the one expected from a Friedmann–Lemaître universe with matter only and the locally measured Hubble parameter.

scholarly journals FORECASTS OF DARK ENERGY CONSTRAINTS FROM BARYON ACOUSTIC OSCILLATIONS

2010 ◽  
Vol 25 (37) ◽  
pp. 3093-3113 ◽  
Author(s):  
YUN WANG
Keyword(s):  
Dark Energy ◽  
Figure Of Merit ◽  
Real Space ◽  
Number Density ◽  
Acoustic Oscillations ◽  
Energy Constraints ◽  
Redshift Survey ◽  
Galaxy Redshift ◽  
Baryon Acoustic Oscillations ◽  
Systematic Noise

The measurement of baryon acoustic oscillations (BAO) from a galaxy redshift survey provides one of the most promising methods for probing dark energy. In this paper, we clarify the assumptions that go into the forecasts of dark energy constraints from BAO. We show that assuming a constant nP0.2/G2(z) (where P0.2 is the real space galaxy power spectrum at k = 0.2 h/ Mpc and redshift z) gives a good approximation of the observed galaxy number density expected from a realistic flux-limited galaxy redshift survey. We find that assuming nP0.2/G2(z) = 10 gives very similar dark energy constraints to assuming nP0.2 = 3, but the latter corresponds to a galaxy number density larger than ~70% at z = 2. We show how the Figure-of-Merit (FoM) for constraining dark energy depends on the assumed galaxy number density, redshift accuracy, redshift range, survey area, and the systematic errors due to calibration and uncertainties in the theory of nonlinear evolution and galaxy biasing. We find that an additive systematic noise of up to 0.4–0.5% per Δz = 0.1 redshift slice does not lead to significant decrease in the BAO FoM.

scholarly journals Forecasting the dark energy measurement with baryon acoustic oscillations: prospects for the LAMOST surveys

2009 ◽  
Vol 394 (4) ◽  
pp. 1775-1790 ◽  
Author(s):  
Xin Wang ◽  
Xuelei Chen ◽  
Zheng Zheng ◽  
Fengquan Wu ◽  
Pengjie Zhang ◽  
...  
Keyword(s):  
Dark Energy ◽  
Energy Measurement ◽  
Acoustic Oscillations ◽  
Baryon Acoustic Oscillations

scholarly journals Probing dark energy with braneworld cosmology in the light of recent cosmological data

2018 ◽  
Vol 27 (02) ◽  
pp. 1850006 ◽  
Author(s):  
Miguel A. García-Aspeitia ◽  
Juan Magaña ◽  
A. Hernández-Almada ◽  
V. Motta
Keyword(s):  
Dark Energy ◽  
Background Radiation ◽  
Big Bang ◽  
Accelerated Expansion ◽  
Joint Analysis ◽  
Brane Tension ◽  
Acoustic Oscillations ◽  
Brane Model ◽  
Baryon Acoustic Oscillations ◽  
The Universe

We investigate a brane model based on Randall–Sundrum scenarios with a generic dark energy component. The latter drives the accelerated expansion at late-times of the universe. In this scheme, extra terms are added into Einstein Field equations that are propagated to the Friedmann equations. To constrain the dark energy equation-of-state (EoS) and the brane tension we use observational data with different energy levels (Supernovae Type Ia, [Formula: see text], baryon acoustic oscillations, and cosmic microwave background radiation distance, and a joint analysis) in a background cosmology. Beside EoS being consistent with a cosmological constant at the [Formula: see text] confidence level for each dataset, the baryon acoustic oscillations probe favors an EoS consistent with a quintessence dark energy. Although we found different lower limit bounds on the brane tension for each dataset, being the most restricted for CMB, there is not enough evidence of modifications in the cosmological evolution of the universe by the existence of an extra dimension within observational uncertainties. Nevertheless, these new bounds are complementary to those obtained by other probes like table-top experiments, Big Bang Nucleosynthesis, and stellar dynamics. Our results show that a further test of the braneworld model with appropriate correction terms or a profound analysis with perturbations, may be needed to improve the constraints provided by the current data.

scholarly journals The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6

2011 ◽  
Vol 415 (3) ◽  
pp. 2892-2909 ◽  
Author(s):  
Chris Blake ◽  
Tamara Davis ◽  
Gregory B. Poole ◽  
David Parkinson ◽  
Sarah Brough ◽  
...  
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Acoustic Oscillations ◽  
Dark Energy Survey ◽  
Baryon Acoustic Oscillations ◽  
Energy Survey

CONSTRAINTS ON VARIABLE CHAPLYGIN GAS MODEL FROM TYPE IA SUPERNOVAE AND BARYON ACOUSTIC OSCILLATIONS

2010 ◽  
Vol 25 (09) ◽  
pp. 737-747 ◽  
Author(s):  
JIANBO LU ◽  
LIXIN XU
Keyword(s):  
Dark Energy ◽  
Chaplygin Gas ◽  
Model Parameters ◽  
Type Ia Supernovae ◽  
Acoustic Oscillations ◽  
Confidence Levels ◽  
Energy Models ◽  
Type Ia ◽  
Baryon Acoustic Oscillations ◽  
Ia Supernovae

We apply the type Ia supernovae union dataset and the baryon acoustic oscillations data at z = 0.2 and z = 0.35 to constrain variable Chaplygin gas (VCG) model as the unification of dark matter and dark energy. It is shown that the confidence levels for VCG model parameters are [Formula: see text]. And it indicates that the values of transition redshift and current deceleration parameter are: [Formula: see text]. In addition, we plot the evolution trajectory of the VCG model in the statefinder parameter r–s plane and show the discrimination between this scenario and other dark energy models.

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