Nikolaos Tetradis

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QuestionAssumed, but not observed directly, dominant contributions tothe energy content of the Universe:1 Dark matter: p = 0 (∼ 25%)2 Dark energy: p < 0 (∼ 70%)Could the acceleration of the cosmological expansion be relatedto the appearance of inhomogeneities in a pressurelesscosmological fluid (dark matter)?N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
Our approachAll the information about the expansion of the Universe isobtained through light signals.Study light propagation in an exact background that mimics aUniverse with structure.Calculate observables: Luminosity distance of a light source afunction of its redshift.P. Apostolopoulos, N. Brouzakis, N. T., E. Tzavaraastro-ph/0603234, JCAP 0606: 009 (2006)N. Brouzakis, N. T., E. Tzavaraastro-ph/0612179, JCAP 0702: 013 (2007)astro-ph/0703586, JCAP 0804: 008 (2008)N. Brouzakis, N. T.arXiv:0802.0859 [astro-ph], Phys. Lett. B 665: 344-348 (2008)N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
Page 2: Figure: 2MASS Galaxy Catalog (more
Page 5: Standard frameworkBasic assumptions
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 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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