Nikolaos Tetradis
Nikolaos Tetradis Nikolaos Tetradis
3.02.5(t,r)/ FRW(t)2.01.51.00.50.7 0.8 0.9 1.0 1.1R(t,r)/R(t,1)Figure: The evolution of the density profile for a central underdensitysurrounded by an overdensity.N. Tetradis University of AthensThe inhomogeneity of the Universe and the cosmological model
Luminosity distance and redshiftConsider photons emitted within a solid angle Ω s by an isotropicsource with luminosity L. These photons are detected by anobserver for whom the light beam has a cross-section A o .The redshift factor is1 + z = ω s= k s0ω o ko0 ,The energy flux f o measured by the observer isf o =L4πD 2 L= L Ω s4π (1 + z) 2 .A oIntegrating the Sachs optical equations allows the determinationof the luminosity distance D L as a function of the redshift z.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: Our approachAll the information abo
- 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
Luminosity distance and redshiftConsider photons emitted within a solid angle Ω s by an isotropicsource with luminosity L. These photons are detected by anobserver for whom the light beam has a cross-section A o .The redshift factor is1 + z = ω s= k s0ω o ko0 ,The energy flux f o measured by the observer isf o =L4πD 2 L= L Ω s4π (1 + z) 2 .A oIntegrating the Sachs optical equations allows the determinationof the luminosity distance D L as a function of the redshift z.N. <strong>Tetradis</strong> University of AthensThe inhomogeneity of the Universe and the cosmological model
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