FIVE-YEAR<i>WILKINSON MICROWAVE ANISOTROPY PROBE</i>OBSERVATIONS: COSMOLOGICAL INTERPRETATION

Komatsu, Eiichiro; Dunkley, Joanna; Nolta, Michael R.; Bennett, C. L.; Gold, B.; Hinshaw, G.; Jarosik, N.; Larson, David; Limon, M.; Page, Lyman A.; Spergel, David N.; Halpern, M.; Hill, Robert S.; Kogut, A.; Meyer, S. S.; Tucker, Gregory S.; Weiland, J. L.; Wollack, Edward J.; Wright, E. L.

doi:10.1088/0067-0049/180/2/330

Cited by 4,624 publications

(4,527 citation statements)

References 449 publications

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“…The accelerated expansion of our Universe is confirmed by many separated cosmological experiments [3][4][5][6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21]. This expansion can be explained in GR by taking into account the dark energy component in the total energy of our Universe.…”

Section: Introductionmentioning

confidence: 54%

Analytic rotating black-hole solutions in N-dimensional f(T) gravity

Nashed

Hanafy

2017

Eur. Phys. J. C

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A non-diagonal vielbein ansatz is applied to the N -dimension field equations of f (T ) gravity. An analytical vacuum solution is derived for the quadratic polynomial f (T ) = T + T 2 and an inverse relation between the coupling constant and the cosmological constant . Since the induced metric has off-diagonal components, it cannot be removed by a mere coordinate transformation, the solution has a rotating parameter. The curvature and torsion scalars invariants are calculated to study the singularities and horizons of the solution. In contrast to general relativity, the Cauchy horizon differs from the horizon which shows the effect of the higher order torsion. The general expression of the energy-momentum vector of f (T ) gravity is used to calculate the energy of the system. Finally, we have shown that this kind of solution satisfies the first law of thermodynamics in the framework of f (T ) gravitational theories.

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Section: Introductionmentioning

confidence: 54%

Analytic rotating black-hole solutions in N-dimensional f(T) gravity

Nashed

Hanafy

2017

Eur. Phys. J. C

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“…In order to find the best fit cosmological parameters for each quintessence model we minimise the function χ 2 total = χ 2 WMAP + χ 2 BAO + χ 2 SN with respect to Ω m h 2 , Ω b h 2 and H 0 . In appendix D of Komatsu et al (2009) it can be seen that including the systematic errors has a very small effect on the ΛCDM parameters but can have a significant effect on dark energy parameters. Using a two parameter equation of state for the dark energy Komatsu et al (2009) found that the parameter constraints weakened considerably after including systematic errors.…”

Section: Discussionmentioning

confidence: 99%

“…In appendix D of Komatsu et al (2009) it can be seen that including the systematic errors has a very small effect on the ΛCDM parameters but can have a significant effect on dark energy parameters. Using a two parameter equation of state for the dark energy Komatsu et al (2009) found that the parameter constraints weakened considerably after including systematic errors. In calculating χ 2 SN in this thesis we have used the covariance matrix for the errors on the SN distance moduli without systematics.…”

Section: Discussionmentioning

confidence: 99%

Simulations of Dark Energy Cosmologies

Jennings

2012

Springer Theses

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source• a link is made to the metadata record in Durham E-Theses• the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. No part of this thesis has been submitted elsewhere for any other degree or qualification.The work of others has been duly acknowledged.The copyright of this thesis rests with the author. No quotations from it should be published without the author's prior written consent and information derived from it should be acknowledged. AbstractFuture galaxy redshift surveys will make high precision measurements of the cosmic expansion history and the growth of structure which will potentially allow us to distinguish between different scenarios for the accelerating expansion of the Universe. In this thesis we study the nonlinear growth of cosmic structure in different dark energy models, using ultra-large volume N-body simulations. We measure key observables such as the growth of large scale structure, the halo mass function and baryonic acoustic oscillations.We study the power spectrum in redshift space in ΛCDM and quintessence dark energy models and test predictions for the form of the redshift space distortions. An improved model for the redshift space power spectrum, including the non-linear velocity divergence power spectrum, is presented. We have found a density-velocity relation which is cosmology independent and which relates the non-linear velocity divergence spectrum to the non-linear matter power spectrum. We provide a formula which generates the non-linear velocity divergence P(k) at any redshift, using only the non-linear matter power spectrum and the linear growth factor at the desired redshift. We also demonstrate for the first time that competing cosmological models with identical expansion histories -one with a scalar field and the other with a time-dependent change to Newton's gravitational constant -can indeed be distinguished by a measurement of the rate at which structures grow.Our calculations show that linear theory models for the power spectrum in redshift space fail to recover the correct growth rate on surprisingly large scales, leading to catastrophic systematic errors. Improved theoretical models, which have been calibrated against simulations, are needed to exploit the exquisitely accurate clustering measurements expected from future surveys.

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“…which is the ratio of the actual baryon fraction, F b = M b /M 500 , in the structure, to the amount of baryons expected from the cosmic baryon fraction, f b = 0.17±0.01 (Komatsu et al 2009). During infall, baryons compress the DM (adiabatic contraction (AC)), and are then subject to radiative processes, giving rise to clumps which condense into stars as described in Li et al (2010) Lucia & Helmi (2008).…”

Section: Structure Formation Modelmentioning

confidence: 99%

Angular Momentum in Dwarf Galaxies

Popolo

2014

Open Astronomy

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Abstract. We study the "angular momentum catastrophe" in the framework of interaction among baryons and dark matter through dynamical friction. By means of Del Popolo (2009) model we simulate 14 galaxies similar to those investigated by van den Bosch, Burkert and Swaters (2001), and calculate the distribution of their spin parameters and the angular momenta. Our model gives the angular momentum distribution which is in agreement with the van den Bosch et al. observations. Our result shows that the "angular momentum catastrophe" can be naturally solved in a model that takes into account the baryonic physics and the exchange of energy and angular momentum between the baryonic clumps and dark matter through dynamical friction.

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FIVE-YEARWILKINSON MICROWAVE ANISOTROPY PROBEOBSERVATIONS: COSMOLOGICAL INTERPRETATION

Cited by 4,624 publications

References 449 publications

Analytic rotating black-hole solutions in N-dimensional f(T) gravity

Analytic rotating black-hole solutions in N-dimensional f(T) gravity

Simulations of Dark Energy Cosmologies

Angular Momentum in Dwarf Galaxies

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