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

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Value <strong>of</strong> β in cz r = H 0 + β cos φSlope β (h km/s/Mpc)1412108642LG frameCMB frame00 20 40 60 80 100 120Inner shell-radius r o (h −1 Mpc)15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.128/143
Dipole directionCMB frame: direction (l d ,b d ) remains within 1σ <strong>of</strong> thebulk flow direction (l,b) = (287 ◦ ± 9 ◦ , 8 ◦ ± 6 ◦ ) found byW<strong>at</strong>kins et al (2009) for 20h −1 ≤ r o ≤ 115h −1 Mpc; forlargest values remains consistent with bulk flowdirection (l,b) = (319 ◦ ± 18 ◦ , 7 ◦ ± 14 ◦ ) <strong>of</strong> Turnbull et al(2012)CMB dipole drops to minimum <strong>at</strong> 40h −1 Mpc but thenincreases and remains 4.0–7.0σ from zero.LG frame: For 20h −1 < ∼ r o< ∼ 45h −1 Mpc while the dipoleis strong, direction is consistently in range(l d ,b d ) = (83 ◦ ± 6 ◦ , −39 ◦ ± 3 ◦ ) but angular position thenwanders once magnitude reduced to residual levels.For r o> ∼ 80h −1 Mpc the typical position <strong>of</strong> residual dipolediffers from th<strong>at</strong> inner dipole by 80 ◦ – 100 ◦ in angle l.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.129/143
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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
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 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: Value of β in cz
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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