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

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Dark flow?Controversial claim <strong>of</strong> bulk flows by Kashlinsky et al(2009,2010) <strong>of</strong> 600 – 1, 000 km s −1 over large scales,coinciding with LG boost direction, using the kinem<strong>at</strong>icSunyaev-Zel’dovich effectClaim to have subtracted all possible primordial dipoles,quadrupoles, octupoles etc, so measurement is madein “cluster rest frames”Not seen by Osborne et al (2011), Hand et al (2012),Lavaux et al (2012) who use different techniquesHowever, we note Kashlinsky modelling <strong>of</strong> clustertemper<strong>at</strong>ure requires use <strong>of</strong> cluster redshift, and anisotropic distance-redshift rel<strong>at</strong>ion is assumeda 1m = a KSZ1m+ a TSZ1m+ a CMB1m+ σ noise√Ncl15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.140/143
Comments on ISW amplitudeIntegr<strong>at</strong>ed Sachs–Wolfe (Rees-Sciama) effect needsrecomput<strong>at</strong>ion in timescape modelCorrel<strong>at</strong>ion <strong>of</strong> radio-galaxies, voids and superclustersetc with CMB positively detected and well established(Boughn and Crittenden 2004, . . . Granett, Neyrinck andSzapudi, 2008)Amplitude <strong>of</strong> effect consistently <strong>of</strong> order 2σ gre<strong>at</strong>er thanLCDM prediction, or 3σ gre<strong>at</strong>er according to recentdetailed calcul<strong>at</strong>ion <strong>of</strong> N<strong>at</strong>hadur, Hotchkiss and Sarkar(2012)Does departure <strong>of</strong> local Hubble flow variance fromΛCDM expect<strong>at</strong>ions may give insights about fe<strong>at</strong>ures <strong>of</strong>inhomogeneities <strong>at</strong> high redshift?15th <strong>Brazilian</strong> <strong>School</strong> on Cosmology and Gravit<strong>at</strong>ion, August 2012 – p.141/143
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Cosmic structure, averaging anddark
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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
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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
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: Large angle CMB anomalies?Anomalies
Page 143: ConclusionApparent cosmic acceler<s
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