Nikolaos Tetradis
Nikolaos Tetradis Nikolaos Tetradis
Observer at the center of a large holeFigure: The distance modulus µ = m − M = 5 log(D L /Mpc) + 25 as afunction of redshift z.a) Green line: FRW cosmology with Ω m = 1, Ω Λ = 0.b) Blue line: FRW cosmology with Ω m = 0.3, Ω Λ = 0.7.c) Red line: LTB cosmology with the observer at the center of an underdenseregion of present size ∼ 800 Mpc.N. Tetradis University of AthensThe inhomogeneity of the Universe and the cosmological model
Observer and source at random positionsProbability DensityProbability Density2402001601208040024020016012080400z=0.5-0.01 0.00 0.01z=1.5-0.01 0.00 0.01Probability DensityProbability Density24020016012080400240200z=1-0.01 0.00 0.01D L/D L, FRW-0.01 0.01160 z=21208040D L/D L, FRW00.00D L/D L, FRWD L/D L, FRWFigure: The distribution of luminosity distances for various redshifts in theLTB Swiss-cheese model for inhomogeneities with length scale 40 h −1 Mpc.N. Tetradis 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: Luminosity distance and redshiftCon
- Page 13 and 14: A similar problem in brane cosmolog
- 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
Observer at the center of a large holeFigure: The distance modulus µ = m − M = 5 log(D L /Mpc) + 25 as afunction of redshift z.a) Green line: FRW cosmology with Ω m = 1, Ω Λ = 0.b) Blue line: FRW cosmology with Ω m = 0.3, Ω Λ = 0.7.c) Red line: LTB cosmology with the observer at the center of an underdenseregion of present size ∼ 800 Mpc.N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
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