Slides of 5 lectures at XV Brazilian School on Cosmology and ...

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Redshift time drift (Sandage–Loeb test)0–0.51 2 3 4 5 6z–1–1.5–2–2.5–3(i)(ii)(iii)H −1 dz0 dτ for the TS model with f v0 = 0.762 (solid line) is compared to three sp<strong>at</strong>ially fl<strong>at</strong>ΛCDM models with the same values <strong>of</strong> (Ω M0,Ω Λ0) as in previous figures.Measurement is extremely challenging. May be feasibleover a 10–20 year period by precision measurements <strong>of</strong>the Lyman-α forest over redshift 2 < z < 5 with nextgener<strong>at</strong>ion <strong>of</strong> Extremely Large Telescopes15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.106/143
Clarkson, Bassett and Lu homogeneity testFor FLRW equ<strong>at</strong>ions, irrespective <strong>of</strong> dark energy modelΩ k0=B[H 0D(z)] 2 = constwhere B(z) ≡ [H(z)D ′ (z)] 2 − 1. ThusC(z) ≡ 1 + H 2 (DD ′′ − D ′2 ) + HH ′ DD ′ = 0for any homogeneous isotropic cosmology, irrespective<strong>of</strong> DE.Clarkson, Bassett and Lu [PRL 101 (2008) 011301] callthis a “test <strong>of</strong> the Copernican principle”. However, it ismerely a test <strong>of</strong> (in)homogeneity.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.107/143
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Cosmic structure, averaging anddark
Page 3 and 4:
Lecture 1What is d
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6df: voids & bubble walls (A. Faira
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Coarse-graining, averaging, backrea
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Layers of coarse-g
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Coarse-graining: further steps(2)
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Dilemma of gravit<
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What is a cosmolog
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Largest typical structuresSurvey Vo
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Scale of st<strong
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I. Coarse-graining at</stro
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Korzyński’s covariant coarse-gra
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Averaging and backreactionAltern<st
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Approach 1: Weak backreactionMuch a
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Zalaletdinov’s macroscopic gravit
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Approach 3: Spatia
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The 3 + 1 decompositionn µN i dtdx
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Buchert-Ehlers-Carfora-Piotrkowska-
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III. Average spati
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Perturbative avera
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The Copernican principleRetain Cope
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What expands? Can
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Semi-tethered latt
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Thought experimentsaverage t = cons
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Finite infinityVirialized=0 θ>0Col
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Better formalism?CEP should be asso
Page 53 and 54:
Two/three scale modelSplit sp<stron
Page 55 and 56: Other ingredients〈R〉 = k v /a v
Page 57 and 58: Dust modelSpecialize to dust only;
Page 59 and 60: Tracker solution limitParameters ǫ
Page 61 and 62: Physical interpretat</stron
Page 63 and 64: Physical interpretat</stron
Page 65 and 66: Dressed cosmological parametersH is
Page 67 and 68: Cosmic coincidence problem solvedSp
Page 69 and 70: Redshift, luminosity distancePerfor
Page 71 and 72: Void fraction, lapse functionThe vo
Page 73 and 74: Age of universeThe
Page 75 and 76: Magnitude of backr
Page 77 and 78: Test 1: SneIa luminosity distancesD
Page 79 and 80: Test 1: SneIa luminosity distancesT
Page 81 and 82: Smale + DLW, MNRAS 413 (2011) 367SA
Page 83 and 84: CMB anisotropiesPower in CMB temper
Page 85 and 86: Photon to baryon rat</stron
Page 87 and 88: Li abundance anomalyBig-bangnucleos
Page 89 and 90: CMB - calibration
Page 91 and 92: Test 3: Baryon acoustic oscill<stro
Page 93 and 94: Dressed “comoving distance” D(z
Page 95 and 96: Equivalent “equat</strong
Page 97 and 98: Sahni, Shafieloo and Starobinsky Om
Page 99 and 100: Sahni, Shafieloo and Starobinsky Om
Page 101 and 102: Baryon Acoustic Oscillat</s
Page 103 and 104: Gaztañaga, Cabre and Hui 0807.3551
Page 105: Redshift time drift (Sandage-Loeb t
Page 109 and 110: Lecture 5Variance of</stron
Page 111 and 112: Result: arXiv:1201.5371v2CMB dipole
Page 113 and 114: Spherical averagesDetermine vari<st
Page 115 and 116: Analysis of COMPOS
Page 117 and 118: Radial variance δH s = (H s − H
Page 119 and 120: But why try the LG frame?From viewp
Page 121 and 122: Angular varianceTwo approaches; fit
Page 123 and 124: Hubble variance: CMB frame15th <str
Page 125 and 126: Angular uncertainties LG frame15th
Page 127 and 128: Value of β in cz
Page 129 and 130: Dipole directionCMB frame: directio
Page 131 and 132: Correlation with r
Page 133 and 134: Redshift-distance anisotropyAs long
Page 135 and 136: Why a strong CMB dipole?Ray tracing
Page 137 and 138: Towards a new formalismFor each she
Page 139 and 140: Large angle CMB anomalies?Anomalies
Page 141 and 142: Comments on ISW amplitudeIntegr<str
Page 143: ConclusionApparent cosmic acceler<s
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