Records from Primordial Gravitational Waves and Cosmic Acceleration in CMB polarization
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1 Records from Primordial Gravitational Waves and Cosmic Acceleration in CMB polarization Carlo Baccigalupi SISSA, Trieste VI Challenges of New Physics in Space, Campos de Jordao, Brazil, May 25-29, 2015
2 Records from Primordial Gravitational Waves and Cosmic Acceleration in CMB polarization Part I: physical processes and cosmological relevance Part II: status of observations Carlo Baccigalupi SISSA, Trieste VI Challenges of New Physics in Space, Campos de Jordao, Brazil, May 25-29, 2015
3 Outline Introduction to SISSA CMB anisotropies Initial conditions and Gravitational Waves Large Scale Structure and Dark Energy Concluding remarks, I
4 The International School for Advanced Studies, Trieste, Italy Main goal: training PhD students to research Interdisciplinary: physics (Astrophysics, Astroparticle, Elementary Particles, Condensed Matters, Statistical Physics), Mathematics, Neuro-sciences About 100 professors, 100 Post-Docs, 200 PhD students Located in Trieste, Italy, one of the places with the highest density of scientific institutions: the international center for theoretical physics, the University of Trieste, the Astronomical observatory in Trieste, research area laboratories
5 The SISSA cosmology group: data analysis for CMB experiments PolarBear (Fabbian, Puglisi): INAF-OATs and SISSA run the Low Frequency Instrument Data Processing Centre, Component Separation for CMB and characterization (Basak, Bielewicz, Castex, Paci) EBEX (Castex, Puglisi) Foreground control and cleaning, B mode power spectrum measurements Planck: Map-making Analysis of maps, foreground cleaning spectrum estimation support for and power CMB satellite/ground-based proposals Data analysis simulations network
6 The SISSA cosmology group: CMB-LSS Cross-Correlations Euclid: CMB-N-body lensing simulations: geodesics (Calabrese, Fabbian) CMB-N-body lensing simulations of cross-correlartions (Bianchini, Calabrese) Herschel: Galaxy formation and evolution (Lapi et al. for the Galaxy Formation group) Cross-correlation with Planck (Bianchini, Bielewicz, Lapi et al. for the Galaxy formation group)
7 CMB anisotropies
8 CMB: where and when? Opacity: λ=1/nσ «horizon where the horizon is the distance at which information get at each time, inverse of the Hubble expansion rate Decoupling: λ horizon Free streaming: λ» horizon Cosmological expansion, Thomson cross section and electron abundance conspire to activate decoupling about years after the Big Bang, at about 3000 K CMB photon temperature
9 A postcard from the big bang From the Stephan Boltzmann law, regions at high temperature should carry high density The latter is activated by perturbations which are intrinsic of the fluid as well as of spacetime Thus, the maps of the CMB temperature is a kind of snapshot of primordial cosmological perturbations
10 From COBE to the Wilkinson Microwave Anisotropy Probe (WMAP) to Planck About 40 years of scientific and technological progresses Lots of experiments, people See lambda.gfsc.nasa.gov
11 CMB physics: Boltzmann equation d photons = gravity + Compton scattering dt d baryons+leptons = gravity + Compton scattering dt
12 CMB physics: Boltzmann equation d neutrinos = gravity + weak interaction dt d dark matter = gravity + weak interaction (?) dt gravity = photons + neutrinos + baryons + leptons + dark matter
13 CMB physics: gravity
14 CMB physics: gravity B Φ Ψ B ±2 ±2 H ±2 T
15 CMB Physics: Compton scattering Compton scattering is anisotropic An anisotropic incident intensity determines a linear polarization in the outgoing radiation At decoupling that happens due to the finite width of last scattering and the cosmological local quadrupole
16 CMB anisotropy: Total Intensity + +
17 CMB anisotropy: polarization Gradient (E): Curl (B): + + +
18 Anisotropies T(θ,φ), Q(θ,φ), U(θ,φ), V(θ,φ) spherical harmonics X(θ,φ)=Σlm almx Yslm(θ,φ) X=T,E,B s=0 for T, 2 for Q and U E and B modes have opposite parity
19 Angular power spectrum T(θ,φ), Q(θ,φ), U(θ,φ), V(θ,φ) spherical harmonics axlm, X=T,E,B information compression Cl=Σm [(almx)(almy)*]/(2l+1)
20 CMB angular power spectrum Angle 200/l degrees
21 Initial conditions and Gravitational Waves
22 Log proper distances CMB physics: initial conditions Log scale factor a
23 Log proper distances CMB physics: initial conditions z=1028 z=104 z=103 T=1015 GeV T=1 ev T=0.1 ev Log scale factor a z=0 T=10-4 ev
24 Present Decoupling Matter radiation equality End of inflation Log proper distances CMB physics: initial conditions z=1028 z=104 z=103 T=1015 GeV T=1 ev T=0.1 ev Log scale factor a z=0 T=10-4 ev
25 CMB physics: initial conditions ~ ~ a Present 2 3/ H Decoupling Matter radiation equality a 1/2 n o ri z o H End of inflation Log proper distances -1 costant z=1028 z=104 z=103 T=1015 GeV T=1 ev T=0.1 ev Log scale factor a z=0 T=10-4 ev
26 CMB physics: initial conditions 2 3/ ~ a H Present ~ a ~ s n o ri z o H Decoupling a 1/2 ale c s al c i g Matter radiation equality ol o m Cos End of inflation Log proper distances -1 costant z=1028 T=1015 GeV z=104 z=103 T=1 ev T=0.1 ev Log scale factor a z=0 T=10-4 ev
27 CMB physics: initial conditions End of inflation Assumed statistics: Gaussianity
28 CMB physics: initial conditions End of inflation Assumed statistics: Gaussianity & Isotropy
29 H-1 costant ica g o ol m Cos H-1 rizo o H a ~ les a c ls n End of inflation Log proper distances CMB physics: initial conditions g n i d or H-1 rec Log scale factor a z=1028 T=1015 GeV
30 CMB physics: initial conditions Harrison Zel-dovich spectrum: End of inflation Harrison Zel dovich spectrum, also known as scale invariant:
31 ica g o ol m Cos a ~ les a c ls o H3-1Horiz H1-1 H2-1 End of inflation Log proper distances CMB physics: initial conditions din r o ec nr g Log scale factor a Z=1028 T=1015 GeV
32 CMB physics: initial conditions Harrison Zel-Dovich spectrum: End of inflation Harrison Zel dovich spectrum, also known as scale invariant:
33 CMB physics: initial conditions Questioning Gaussianity: End of inflation Finite correlation: Usually expressed in terms of second order correction:
34 CMB physics: initial conditions Non-scalar metric modes: Vectors decay Scalars and tensors keep constant End of inflation For total intensity, tensors they contribute on all scales:
35 CMB physics: initial conditions Non-scalar metric modes: Vectors decay Scalars and tensors keep constant End of inflation Tensors are not substained by radiation pressure when sub-horizon, implying rapid diffusion damping Super-horizon tensor perturbation cannot be recorded in polarisation Polarisation CMB anisotropies from tensors peak on the angular scale corresponding to the width of the last scattering region, about 1 degree in the sky: GWs wavelength contributing to CMB polarisation
36 The B-modes record GWs monochromatically in angle
37 The B-modes record GWs mono-chromatically in angle Gravitati on sources, al waves not sup d p Horizon s iffuse out rapidly orted by below th cale, abo e ut 1 degr ee in the sky
38 The B-modes record GWs mono-chromatically in angle Gravitati on sources, al waves not sup d p Horizon s iffuse out rapidly orted by below th cale, abo e ut 1 degr ee in the sky 0 Mpc ute 1 t u o b ib ts for a hts to contr s a l e g im pling t ger wavelen u o c e D for lon e m i t No
39 The B-modes record GWs mono-chromatically in angle Gravitati on sources, al waves not sup d p Horizon s iffuse out rapidly orted by below th cale, abo e ut 1 degr ee in the sky 1 0 Mpc ute 1 t u o b ib ts for a hts to contr s a l e g im pling t ger wavelen u o c e D for lon e m i t No
40 CMB angular power spectrum Angle 200/l degrees
41 CMB angular power spectrum Acoustic oscillations Primordial power Angle 200/l degrees Gravitational waves
42 Large Scale Structure and Dark Energy
43 LSS effects on CMB Forming structures???????? Last scattering
44 Categories for LSS effects on CMB Re-scattering Gravitation
45 Categories for LSS effects on CMB Re-scattering Re-ionization Gravitation Time evolution of the metric tensor Deflection
46 Reionization
47 CMB anisotropy: reionization e- ee-
48 CMB anisotropy: reionization e- ee-
49 CMB anisotropy: reionization e- ee- H-1
50 Planck 2015: reionization epoch
51 Integrated Sachs-Wolfe
52 Integrated Sachs-Wolfe Forming structures Last scattering Sachs & Wolfe 1967
53 Integrated Sachs-Wolfe Forming structures Last scattering Sachs & Wolfe 1967
54 Integrated Sachs-Wolfe Forming structures Last scattering Sachs & Wolfe 1967
55 Integrated Sachs-Wolfe Forming structures H-1 Last scattering Sachs & Wolfe 1967
56 Integrated Sachs-Wolfe Forming structures m Sa e pl va e nc ria Last scattering Sachs & Wolfe 1967
57 Cross-correlating with LSS
58 Cross-correlating with LSS Perturbation statistics and dynamics early Universe
59 Cross-correlating with LSS Geometry and perturbation dynamics dark energy effects
60 Planck 2015: non-zero ISW-LSS Cross-Spectra at 4σ
61 CMB lensing
62 T CMB lensing Forming structures - lenses Last scattering Bartelmann, Schneider 2001, Hu 2000
63 CMB lensing EB Forming structures - lenses Last scattering Kamionkowski, Kosowsky & Stebbins, Zaldarriaga & Seljak1998
64 CMB lensing T EB Forming structures - lenses acceleration Last scattering
65 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
66 Dark energy density ia t io n r te t a m ra d Energy density ρ(z) dark energy z
67 Constant Dark Energy (Λ) 0.5 ia t io n r te t a m constant w ra d Energy density ρ (1+z)3[1+w] 104 z
68 Scaling Dark Energy 0.5 ia t io n r te t a m constant w ra d Energy density ρ (1+z)3[1+w] 104 z
69 Early Dark Energy Energy density ρ exp{3 0z [1+w(z)]dz/(1+z)} variable w z
70 Messy Dark Energy Energy density ρ exp{3 0z [1+w(z)]dz/(1+z)} variable w z
71 The promise of CMB lensing Energy density Matter radiation equivalence CMB last scattering Dark energy matter equivalence Dark energy domination dark energy z
72 Structure formation Energy density The promise of CMB lensing Matter radiation equivalence CMB last scattering Dark energy matter equivalence Dark energy domination 0.5 dark energy z
73 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
74 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
75 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
76 Lensing probability Energy density Lensing strength recording the cosmic density at the onset of acceleration dark energy Cosmological constant 1 3 z
77 CMB lensing Acquaviva et al. 2004
78 CMB lensing Geometry Acquaviva et al. 2004
79 CMB lensing Perturbation dynamics Acquaviva et al. 2004
80 Early dark energy and CMB lensing Acquaviva & Baccigalupi 2006
81 CMBreaking projection degeneracy Acquaviva & Baccigalupi 2006
82 Planck lensing 2015
83 Planck lensing 2015
84 Lensing-LSS Cross-Correlations Bianchini et al. 2014, 2015 in preparation
85 Lensing-LSS Cross-Correlations Bianchini et al. 2014, 2015 in preparation
86 CMB-N-body Lensing Calabrese et al. 2014, 2015 in preparation
87 CMB angular power spectrum Acoustic oscillations Primordial power Angle 200/l degrees Gravitational waves
88 CMB angular power spectrum ISW Acoustic oscillations Primordial power Lensing Reionization Angle 200/l degrees Gravitational waves
89 Planck 2015 CMB
90 Planck 2015 TT power spectrum
91 Planck 2015 TE and EE power spectra
92 Planck 2015 BB power spectra
93 Concluding remarks, I Effects from the Early Universe and Large Scale Structure affect large parts of CMB anisotropies, and directly compete for detection, for example in the B-modes Measurements of the abundance of primordial Gravitational Waves, and constraints on the Dark Energy dynamics must proceed jointly in the analysis of data from operating and future high resolution and sensitivity probes, LSS surveys Cross-correlation studies gathering relevance, large scale simulations CMB LSS experiments being implemented...
94 Planck The scientific results that we present today are a product of the Planck Collaboration, including individuals from more than 100 scientific institutes in Europe, the USA and Canada C IT A IC AT U N IV E R SIT À D E G L I D I M IL A N O STU DI ABabcdfghiejkl Planck is a project of the European Space Agency, with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark.
95 Backup slides
96 Extension I: CMB-N-body lensing
97 CMB-N-Body lensing
98 CMB-N-body lensing: do we really need it? Do we have a satisfactory statistics in semianalytic prescriptions for CMB lensing? Do we have an understanding of mildly and full non-linear Dark Matter clustering in Dark Energy models? Can we learn about simulations trying to get the signal right in particular at high resolution? Do we need simulations for understanding cross-correlation studies?...
99 CMB-N-body lensing Carbone et al. 2008, 2009, 2013
100 CMB-N-body lensing ray-tracing: Born or non-born? Hilbert et al. 2009
101 CMB-N-body lensing ray tracing Hilbert et al. 2009, Calabrese et al. 2013
102 CMB-N-body lensing Carbone et al. 2008, 2009, 2013
103 CMB-N-body lensing Carbone et al. 2008, 2009, 2013
104 CMB-N-body lensing Carbone et al. 2008, 2009, 2013
105 CMB-N-body lensing Carbone et al. 2008, 2009, 2013
106 CMB-N-body lensing: first inspection of non-lcdm cosmologies Baldi et al. 2012, Carbone et al. 2013
107 CMB-N-body lensing: first inspection of non-lcdm cosmologies Baldi et al. 2012, Carbone et al. 2013
108 CMB-N-body lensing: gridding issues Carbone et al. 2008, 2009, 2013
109 CMB-N-body lensing: skewed statistics in the CMB lensed/non-lensed maps Carbone et al. 2008, 2009, 2013
110 CMB-N-body lensing: learning lessons on N-body Carbone et al. 2008, 2009, 2013
111 CMB lensing and sub-orbital CMB probes: extraction Fantaye et al. 2012
112 CMB lensing and sub-orbital CMB probes: extraction Convergence estimation With foreground cleaning Convergence estimation Without foreground cleaning Fantaye et al. 2012
113 CMB-N-body lensing reconstruction Antolini, et al. 2014
114 CMB-N-body lensing reconstruction Antolini, et al. 2014
115 Concluding remarks Is lensing relevant for Dark Energy? Does the signal keep its promise? Do we need CMB-N-body lensing? Do we have the technology for simulating it? Do we have a complete understanding of the effects of details in the simulations in the signal we see? Can we start simulating cross-correlation studies on the way to Euclid?...
116 Concluding remarks Is lensing relevant for Dark Energy? Yes, it is. Does the signal keep its promise? Yes, it does. Do we need CMB-N-body lensing? Well...yes. Do we have the technology for simulating it? Yes...still limited by present simulations, but it works. Do we have a complete understanding of the effects of details in the simulations in the signal we see? No. We still need to distinguish between physical effects/nbody details/gridding issues at high resolution. Can we start simulating cross-correlation studies on the way to Euclid? Oh yes, we should......
117 Extension II: A mini-dark Energy Course
118 Fighting the cosmological constant Gµν=8πTµν
119 Fighting the cosmological constant geometry Gµν+Λg µν=8πtµν +Vgµν quantum vacuum
120 Fighting the cosmological constant Λ:???
121 Fighting the cosmological constant V:M Planck??? 4
122 Fighting the cosmological constant Λ:??? Λ-V /M Planck= V:M Planck??? 4
123 (Boh?) 2 Why so small with respect to any other known energy scale in physics? Why comparable to the matter energy density today?
124 ia t io n r te t a m ra d Energy density Dark Energy dark energy z
125 ia t io n r te t a m ra d Energy density Dark Energy dark energy z
126 ia t io n r te t a m ra d Energy density Dark Energy dark energy z
127 ia t io n r te t a m ra d Energy density Dark Energy dark energy z
128 ia t io n r te t a m ra d Energy density Dark Energy dark energy z
129 Parametrizing cosmic acceleration is ia t io n r te t a m ra d Energy density ρ(z) dark energy z
130 parametrizing cosmic density 0.5 ia t io n r te t a m constant w ra d Energy density ρ (1+z)3[1+w] 104 z
131 Parametrizing cosmic density Energy density ρ exp{3 0z [1+w(z)]dz/(1+z)} variable w z
132 Cosmological expansion and CMB: projection z D= H0-1 0 w D dz [ΣiΩi(1+z)3(1+wi)]1/2
133 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
134 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
135 Constraining the expansion with distances z D= H dz [ΣiΩi(1+z)3(1+wi)]1/2
136 Constraining Dark Energy: models w w=w0-wa(1-a)=w0+(1-a)(w -w0) -w a w -1 w a=1/(1+z) Chevallier & Polarski 2001, Linder 200
137 -1 w Constraining Dark Energy: binning a=1/(1+z) Crittenden & Pogosian 2006, Dick et al. 2006,Said et al. 2
138 Constraining Dark Energy: latest pre-planck constraints Said et al. 2013
139 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
140 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
141 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
142 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
143 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
144 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
145 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
146 er t t ma rad iat ion Energy density The promise of CMB lensing dark energy z
147 Lensing probability Energy density Lensing strength recording the cosmic density at the onset of acceleration Cosmological constant z
148 Lensing probability Energy density Lensing strength recording the cosmic density at the onset of acceleration dark energy Cosmological constant z
149 T CMB lensing Forming structures - lenses Last scattering Bartelmann, Schneider 2001, Hu 2000
150 T CMB lensing Forming structures - lenses Last scattering Bartelmann, Schneider 2001, Hu 2000
151 T CMB lensing Forming structures - lenses Last scattering Bartelmann, Schneider 2001, Hu 2000
152 Early dark energy and CMB lensing Acquaviva & Baccigalupi 2006
153 CMBreaking projection degeneracy Acquaviva & Baccigalupi 2006
154 Expanding universe => CMB compression in the early stages of an expanding universe causes lots of radiation arising from thermonuclear explosions Reactions are rapid enough to achieve thermalization and a black body spectrum It is possible to compute the rarefaction caused by the expansion since that epoch The relic radiation is predicted to peak in microwaves, temperature of a few Kelvin, known today as the Cosmic Microwave Background (CMB, Gamow et al. 1948) George Gamow, three years old in Odessa, Ukraine, 1907
155 Discovery
156 COsmic Background Explorer
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