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

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Coarse-graining: final steps(4) → (5) (bound galaxy clusters → expandingwalls/filaments)New ingredient: expanding space(1) + (5) → (6) (voids + walls/filaments → universe)New ingredient: “building blocks” themselves areexpandingEffective hierarchyg stellarµν → g galaxyµν → g clusterµν → g wallµν.g voidµν⎫⎪⎬⎪⎭ → guniverse µνHow does 〈T µ ν(g x µν)〉 → T µ ν(g y µν) <strong>at</strong> each step?15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.12/143
Dilemma <strong>of</strong> gravit<strong>at</strong>ional energy. . .In GR spacetime carries energy & angular momentumG µν = 8πGc 4 T µνOn account <strong>of</strong> the strong equivalence principle, T µνcontains localizable energy–momentum onlyKinetic energy and energy associ<strong>at</strong>ed with sp<strong>at</strong>ialcurv<strong>at</strong>ure are in G µν : vari<strong>at</strong>ions are “quasilocal”!Newtonian version, T − U = −V , <strong>of</strong> Friedmann equ<strong>at</strong>ionȧ 2a 2 + kc2a 2 = 8πGρ3where T = 1 2 mȧ2 x 2 , U = − 1 2 kmc2 x 2 , V = − 4 3 πGρa2 x 2 m;r = a(t)x.15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.13/143
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: Coarse-graining: further steps(2)
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
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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
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Test 1: SneIa luminosity distancesD
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Test 1: SneIa luminosity distancesT
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Smale + DLW, MNRAS 413 (2011) 367SA
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CMB anisotropiesPower in CMB temper
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Photon to baryon rat</stron
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Li abundance anomalyBig-bangnucleos
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CMB - calibration
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Test 3: Baryon acoustic oscill<stro
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Dressed “comoving distance” D(z
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Equivalent “equat</strong
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Sahni, Shafieloo and Starobinsky Om
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Sahni, Shafieloo and Starobinsky Om
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Baryon Acoustic Oscillat</s
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Gaztañaga, Cabre and Hui 0807.3551
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Redshift time drift (Sandage-Loeb t
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Clarkson, Bassett and Lu homogeneit
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Lecture 5Variance of</stron
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Result: arXiv:1201.5371v2CMB dipole
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Spherical averagesDetermine vari<st
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Analysis of COMPOS
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Radial variance δH s = (H s − H
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But why try the LG frame?From viewp
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Angular varianceTwo approaches; fit
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Hubble variance: CMB frame15th <str
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Angular uncertainties LG frame15th
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Value of β in cz
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Dipole directionCMB frame: directio
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Correlation with r
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Redshift-distance anisotropyAs long
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Why a strong CMB dipole?Ray tracing
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Towards a new formalismFor each she
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Large angle CMB anomalies?Anomalies
Page 141 and 142:
Comments on ISW amplitudeIntegr<str
Page 143:
ConclusionApparent cosmic acceler<s
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