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

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Boosts and spurious monopole varianceH s determined by linear regression in each shellH s =(Ns∑i=1(cz i ) 2σ 2 i) (Ns∑i=1cz i r iσ 2 i) −1,Under boost cz i → cz i ′ = cz i + v cosφ i for uniformlydistributed d<strong>at</strong>a, linear terms cancel on opposite sides<strong>of</strong> skyH ′ s − H s∼(Ns∑i=1(v cosφ i ) 2σ 2 i= 〈(v cos φ i) 2 〉〈cz i r i 〉∼) (Ns∑v2i=12H 0〈r 2 i 〉cz i r iσ 2 i) −115th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.120/143
Angular varianceTwo approaches; fit1. McClure and Dyer (2007) method – can look <strong>at</strong> highermultipoles∑ Ni=1H α =W i α cz i ri−1∑ Nj=1 W j αwhere with cos θ i = ⃗r grid · ⃗r i , σ θ= 25 ◦ (typically)W i α =1√2πσθexp( −θ2i2σ 2 θ)2. Simple dipoleczr = H 0 + b cos φ15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.121/143
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Cosmic structure, averaging anddark
Page 3 and 4:
Lecture 1What is d
Page 5 and 6:
6df: voids & bubble walls (A. Faira
Page 7 and 8:
Coarse-graining, averaging, backrea
Page 9 and 10:
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
Page 17 and 18:
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
Page 29 and 30:
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
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Dressed cosmological parametersH is
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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 and 116: Analysis of COMPOS
Page 117 and 118: Radial variance δH s = (H s − H
Page 119: But why try the LG frame?From viewp
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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