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

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Li abundance anomaly(i)(ii)Expected abundances for different values <strong>of</strong> theparameter η 10≡ 10 10 η Bγ(left), and measurements(right) (Steigman 2006), with 1σ uncertainties.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.86/143
Li abundance anomalyBig-bangnucleosynthesis, lightelement abundancesand WMAP with ΛCDMcosmology.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.87/143
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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<
Page 15 and 16:
What is a cosmolog
Page 17 and 18:
Largest typical structuresSurvey Vo
Page 19 and 20:
Scale of st<strong
Page 21 and 22:
I. Coarse-graining at</stro
Page 23 and 24:
Korzyński’s covariant coarse-gra
Page 25 and 26:
Averaging and backreactionAltern<st
Page 27 and 28:
Approach 1: Weak backreactionMuch a
Page 29 and 30:
Zalaletdinov’s macroscopic gravit
Page 31 and 32:
Approach 3: Spatia
Page 33 and 34:
The 3 + 1 decompositionn µN i dtdx
Page 35 and 36: Buchert-Ehlers-Carfora-Piotrkowska-
Page 37 and 38: III. Average spati
Page 39 and 40: Perturbative avera
Page 41 and 42: The Copernican principleRetain Cope
Page 43 and 44: What expands? Can
Page 45 and 46: Semi-tethered latt
Page 47 and 48: Thought experimentsaverage t = cons
Page 49 and 50: Finite infinityVirialized=0 θ>0Col
Page 51 and 52: 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: Photon to baryon rat</stron
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 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
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ConclusionApparent cosmic acceler<s
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