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

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Supernovae system<strong>at</strong>ics0.7Gold (167 SneIa)0.7SDSS−II 1st year (272 SneIa)0.60.60.50.5Ω m00.40.3Ω m00.40.30.20.20.10.1056 58 60 62 64 66 68H0056 58 60 62 64 66 68H0MLCS17 (219 SneIa)MLCS31 (219 SneIa)0.60.60.50.5Ω m00.40.3Ω m00.40.30.20.20.10.1056 58 60 62 64 66 68H0056 58 60 62 64 66 68H015th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.82/143
CMB anisotropiesPower in CMB temper<strong>at</strong>ure anisotropies versus angular size <strong>of</strong> fluctu<strong>at</strong>ion on sky15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.83/143
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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)
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: Smale + DLW, MNRAS 413 (2011) 367SA
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 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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