Cosmology with CMB & LSS:

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1 Cosmology with CMB & LSS: the Early universe VSP08 lecture 4 (May 12-16, 2008) Tarun Souradeep I.U.C.A.A, Pune, India

2 Ω +Ω +Ω +Ω + Ω +... = m DE K r r The Cosmic Triangle (Ostriker & Steinhardt) Ω = 0 0K

3 Planck Surveyor Satellite European Space Agency: Launch 2008

4 Planck Satellite on display at Cannes, France (Feb. 1, 2007)

5 Planck Surveyor mission PLANCK frequency channels and independent detectors per channels allow exquisite foreground removal & power Frequency (in GHz) Average ΔT N /T per pixel (in μk) Average ΔT N per pixel (in μk) No. of detectors ( Tuhin Ghosh, R Saha, S. Prunet, TS: in progress)

6 CMB Maps at Planck Frequencies 30 GHz 44 GHz 70 GHz 100 GHz 143 GHz 217 GHz 353 GHz 545 GHz 857 GHz

7 Near future : High resolution C l (SPT) CMB Task force report 2005

8 Gravitational Instability Mildly Perturbed universe at z=1100 Present universe at z=0 Cosmic matter content Ω Ω Ω tot b DM Ω Λ H 0 (credit: Virgo simulations)

9 Gravitational Instability Time Cosmological constant + cold dark matter Standard cold dark matter (fig: Virgo simulations) (quarter size ) (half size) expansion ( now )

10 Power spectrum of mass distribution

11 Characterizing the mass distribution power spectrum Var(R) vs. R Measure the variance in the total mass var(m) enclosed in spheres of a given radius R thrown randomly in the cosmos.

12 Power spectrum of mass distribution ( Tegmark et al. 2004) k eq : k eq τ eq =1

13 Sensitivity to curvature

14 Sensitivity to Baryonic matter fraction

15 Sensitivity to Dark energy fraction

16 Sensitivity to Dark matter fraction

17 CMB + Cmbgg OmOl LSS (credit: Tegmark)

18 Ω +Ω +Ω +Ω + Ω +... = m DE K r r The Cosmic Triangle Ω = 0.3 0m (Ostriker & Steinhardt) Ω = 0 0K

19 Weighing the Neutrinos

20 Cosmological constraints on ν mass 3-ν degenerate mass Ω ν = 3 m ν /(94.0 ev) f ν = Ω ν /Ω DM m ν m ν m ν (95% CL) < 1.0 ev < 0.4 ev < 0.16 ev (MacTavish et al. astro-ph/ )

21 Gravitational Instability Mildly Perturbed universe at z=1100 Present universe at z=0 Cosmic matter content Ω Ω Ω tot b DM Ω Λ H 0

22 Present distribution of matter Few Gpc. SLOAN DIGITAL SKY SURVEY (SDSS)

23 One little telltale bump!! ξ() r = δρ( r) δρ( r ) 1 2 A small excess in correlation at 150 Mpc.! SDSS survey (astro-ph/ ) (Einsentein et al. 2005) 150 Mpc.

24 Acoustic Baryon oscillations in the matter correlation function!! 2-point correlation of density contrast 105 h Undeniable proof of Gravitational instability mechanism for structure formation (from adiabatic initial perturbations)!!! 150 Mpc. The same CMB oscillations at low redshifts!!! SDSS survey (astro-ph/ ) (Einsentein et al. 2005)

25 Ripples in the different constituents

26 What s the next frontier

27 Quantum fluctuations super adiabatic amplified by inflation (rapid expansion) Galaxy & Large scale Structure formation Via gravitational instability Early Universe The Cosmic screen Present Universe Who pinged the Cosmic drum?

28 Inflation a paradigm in search of a model A phase of rapid expansion in the scale factor of the universe Hubble Radius time

29 Generic Inflation model A scalar field displaced from the minima of its potential Linde s chaotic inflation φ + 3 Hφ + V = 0 3 ρ φ 1 2 H 2 = = 2 +V p = 1 φ 2 V 2

30 Generic Inflation model A scalar field displaced from the minima of its potential Deceleration = 3 2 : q = a ah ( ρ + 3 p) ( φ 2 V ) = 3 ρ ρ 2 Inflation φ 2 / V < 1

31 Generation of fluctuations " DeSitter" q.fluc.: δφ δφ ( ) H No. of e - folds : N = H dt δn = Hδt e = H φ δφ

32 String theory Landscape: Non trivial skiing slopes

33 Early Universe in CMB The Background universe Homogeneous & isotropic space: Cosmological principle Flat (Euclidean) Geometry The nature of initial/primordial perturbations Power spectrum : Nearly Scale invariant /scale free form Spin characteristics: (Scalar) Density perturbations Type of scalar perturbation: Adiabatic -- no entropy fluctuations Underlying statistics: Gaussian

34 CMB Polarization Thompson scattering at redshift z=1100 (surface of last scattering) generates a linear polarization pattern in the CMB sky. Two polarization modes E&B Four CMB spectra : C l TT, C l EE,C l BB,C l TE Density (scalar) perturbations generate only E mode polarization. E-mode μ K Gravitational waves generate both the modes in comparable amounts. B-mode μ K B-mode measures cosmic gravity wave background.

35 Thompson scattering of the CMB anisotropy quadrupole at the surface of last scattering generates a linear polarization pattern in the CMB. (Fig:Hu & White, 97)

36 E modes (Gradient) B modes (Curl)

37 Polarization: E modes and B modes E Modes: Gradient of the polarization Produced by both scalar and tensor modes Have been detected B Modes: Curl of the polarization Produced only by tensor modes...or gravitational lensing...or foregrounds...or systematics Expected from inflation Have not been detected E B A detection of primordial sourced B modes would provide important evidence for, and determine the energy scale of Inflation

38 NASA/WMAP science team 2006

39 (Boomerang 2003, WMAP-3) (not so) Current status of CMB Spectra Null BB: Awaiting direct signature of tensor perturbations, a.k.a. Out of phase location of peaks in EE, TE relative to TT implies adiabatic initial perturbations!!! cosmic gravity waves!!! Proof of inflation!

40 Current status of CMB Spectra (QUaD results today)

41 CMB Task force report 2005

42 CMB Task force report 2005

43 WMAP-1yr Timeline of CMB experiments now WMAP-3yr WMAP-8yr Planck (ESA) Next Gen. space CMBPOL CMB Task force report 2005

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