- Page 1 and 2:
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
- Page 11 and 12:
Coarse-graining: further steps(2)
- Page 13 and 14:
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 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 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: Towards a new formalismFor each she
- Page 141 and 142: Comments on ISW amplitudeIntegr<str
- Page 143: ConclusionApparent cosmic acceler<s