Nikolaos Tetradis

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Probability Density100806040200z=0.5-0.04 -0.02 0.00 0.02Probability Density100806040200z=1-0.04 -0.02 0.00 0.02D L/D L, FRWD L/D L, FRWProbability Density100806040200z=1.5-0.04 -0.02 0.00 0.02Probability Density100806040200z=2-0.04 -0.02 0.00 0.02D L/D L, FRWD L/D L, FRWFigure: Same as before for a characteristic scale of 400 h −1 Mpc.N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
A similar problem in brane cosmologyIdentify the Universe with a hypersurface (brane) infive-dimensional space-time. Low-energy gravity is localizednear the brane (Randall, Sundrum (1999)).Assume an inhomogeneous energy distribution along the fourthspatial dimension. Is accelerated expansion possible along thebrane?For an arbitrary energy distribution, accelerated expansionrequires negative pressure either on the brane or in the bulk.This holds even when corrections, such as an induced gravityterm on the brane, or a Gauss-Bonnet term in the bulk, are takeninto account.P. Apostolopoulos, N. T.astro-ph/0604014, Phys. Rev. D 74: 064021 (2006)P. Apostolopoulos, N. Brouzakis, N. T., E. TzavaraarXiv:0708.0469, Phys. Rev. D 76: 084029 (2007)N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
Page 2: Figure: 2MASS Galaxy Catalog (more
Page 5 and 6: Standard frameworkBasic assumptions
Page 7 and 8: Our approachAll the information abo
Page 9 and 10: Luminosity distance and redshiftCon
Page 11: Observer and source at random posit
Page 15 and 16: Basic relationsAction∫S =d 4 x
Page 17 and 18: Static spherically symmetric config
Page 19 and 20: Compact astrophysical objects made
Page 21 and 22: Astrophysical objects made of neutr
Page 23 and 24: Sloan Digital Sky Survey (2005)Figu
Page 25 and 26: Ansatz for the metricds 2 = a 2 (τ
Page 27 and 28: Equations of motion for several non
Page 29 and 30: Time renormalization group (Pietron
Page 31 and 32: The non-zero components of the effe
Page 33 and 34: In this way we obtain∂ η P ab (k
Page 35 and 36: 7Density-Density Power Spectra at z
Page 37 and 38: 1.7BAO Power Spectra at z=0 (β=0.1
Page 39 and 40: wz0.40.60.81.01.41.62 4 6 8 10 zFig
Page 41 and 42: ∆k i k i,lin0.0150.0100.005(2)0.0
Page 43 and 44: Growing neutrino quintessence i , q
Page 45: ConclusionsThe inhomogeneities in t

Nikolaos Tetradis

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