Nikolaos Tetradis
Nikolaos Tetradis Nikolaos Tetradis
1.9BAO Baryonic Matter Density-Density Power Spectra at z=0 for different β1.81.71.61.5PS1.41.31.21.110.90.05 0.075 0.1 0.125 0.15 0.175 0.2 0.225 0.25 0.275 0.3k (h/Mpc)linear (β=0)TRG (β=0)linear (β=0.05)TRG (β=0.05)linear (β=0.1)TRG (β=0.1)Figure: Baryonic matter density-density spectra for various β at z = 0,normalized with respect to the a smooth spectrum.N. Tetradis University of AthensThe inhomogeneity of the Universe and the cosmological model
1.7BAO Power Spectra at z=0 (β=0.1)1.61.51.4PS1.31.21.110.90.05 0.075 0.1 0.125 0.15 0.175 0.2 0.225 0.25 0.275 0.3k (h/Mpc)P ccddP ccdvP ccvvP bbddP bbdvP bbvvFigure: Spectra for β = 0.1 at z = 0, normalized with respect to a smoothspectrum.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 and 10: Luminosity distance and redshiftCon
- Page 11 and 12: Observer and source at random posit
- 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: 7Density-Density Power Spectra at z
- 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
1.7BAO Power Spectra at z=0 (β=0.1)1.61.51.4PS1.31.21.110.90.05 0.075 0.1 0.125 0.15 0.175 0.2 0.225 0.25 0.275 0.3k (h/Mpc)P ccddP ccdvP ccvvP bbddP bbdvP bbvvFigure: Spectra for β = 0.1 at z = 0, normalized with respect to a smoothspectrum.N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
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