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

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(a) 1: 0−12.5 h −1 Mpc N = 92. (b) 2: 12.5−25 h −1 Mpc N = 505.(c) 3: 25−37.5 h −1 Mpc N = 514. (d) 4: 37.5−50 h −1 Mpc N = 731.(e) 5: 50−62.5 h −1 Mpc N = 819. (f) 6: 62.5−75 h −1 Mpc N = 562.(g) 7: 75−87.5 h −1 Mpc N = 414. (h) 8: 87.5−100 h −1 Mpc N = 304.(i) 9: 100−112.5 h −1 Mpc N = 222. (j) 10: 112.5−156.25 h −1 Mpc N = 280.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.116/143(k) 11: 156.25−417.4 h −1 Mpc N = 91.
Radial variance δH s = (H s − H 0 )/H 0Two choices <strong>of</strong> shell boundaries (closed and opencircles); for each choice d<strong>at</strong>a points uncorrel<strong>at</strong>edAnalyse linear Hubble rel<strong>at</strong>ion in rest frame <strong>of</strong> CMB;Local Group (LG); Local Sheet (LS). LS result veryclose to LG result.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.117/143
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Cosmic structure, averaging anddark
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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
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Two/three scale modelSplit sp<stron
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Other ingredients〈R〉 = k v /a v
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Dust modelSpecialize to dust only;
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Tracker solution limitParameters ǫ
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Physical interpretat</stron
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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 and 106: Redshift time drift (Sandage-Loeb t
Page 107 and 108: Clarkson, Bassett and Lu homogeneit
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: Analysis of COMPOS
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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