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

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Correl<strong>at</strong>ion with CMB dipole as r o variedCorrel<strong>at</strong>ion coefficient0-0.2-0.4-0.6-0.8LG inner sphere, no I.V. wtgLS inner sphere, no I.V. wtgLG outer sphere, no I.V. wtgLS outer sphere, no I.V. wtgLG outer sphere, I.V wtgLS outer sphere, I.V. wtg-110 20 30 40 50 60 70 80 90Distance cut r 0 (h -1 Mpc)15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.132/143
Redshift-distance anisotropyAs long as T ∝ 1/a, where a 0/a = 1 + z for someappropri<strong>at</strong>e average, not necessarily FLRW, then smallchange, δz, in the redshift <strong>of</strong> the surface <strong>of</strong> photondecoupling – due to foreground structures – will inducea CMB temper<strong>at</strong>ure increment T = T 0+ δT , withδTT 0=−δz1 + z decWith z dec = 1089, δT = ±(5.77 ± 0.36) mK represents anincrement δz = ∓(2.31 ± 0.15) to last sc<strong>at</strong>teringProposal: r<strong>at</strong>her than origin<strong>at</strong>ing in a LG boost the±5.77 mK dipole is due to a small anisotropy in thedistance-redshift rel<strong>at</strong>ion on scales < ∼ 65h −1 Mpc.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.133/143
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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
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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
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Redshift, luminosity distancePerfor
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Void fraction, lapse functionThe vo
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Age of universeThe
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Magnitude of backr
Page 77 and 78:
Test 1: SneIa luminosity distancesD
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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 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: Correlation with r
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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