The cosmic background radiation II: The WMAP results. Alexander Schmah

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1 The cosmic background radiation II: The WMAP results Alexander Schmah

2 General Aspects - WMAP measures temperatue fluctuations of the CMB around K - Reason for the temperature fluctuations are density fluctuation in the early universe - The CMB comes from the age of the decoupling of the photons from the matter - The CMB data is described with cosmological models

3 WMAP: Overview Wilkinson Microwave Anisotropy Probe: WMAP -Named after Dr. David Wilkinson, pioneer in the study of CMB and member of the science team, died in September WMAP weight: 840 kg -Angular resolution: Sensitivity: 20 K/(0.3 )2

4 Launch Launch of the Delta II rocket on 30 June 2001

5 Measuring position million km away from earth - scans ~30% of the sky per day - full sky coverage after ½ year Orbit around the second Lagrange point (L2) of the Earth-Sun system

6 WMAP: Detectors I

7 WMAP: Detectors II -Two back to back symmetric telescopes -Differential microwave radiometers - Angle between opposite feed horns: ~ 141

8 Frequency Bands K-band: ~22 GHz (13.6 mm) (1) Ka-band: ~30 GHz (10.0 mm) (1) Q-band: ~40 GHz (7.5 mm) (2) V-band: ~60 GHz (5.0 mm) (2) W-band: ~90 GHz (3.3 mm) (4)

9 Thermal spectrum K-band W-band

10 Cosmic Background charged particles interacting with magnetic fields hot gas (thermal Bremsstrahlung) thermal emission

11 Map making DT =T A T B T A =DT T B Measured signal T 1 A =DT 1 T B1 T 2 A =DT 2 T B 2.. T n A =DT n T B n Iterative procedure Absolute temperature estimated n 1 T A = T i A n i =1

12 Map projection

13 Scan strategy

14 Observation Map

15 Galactic Plane Map

16 Dipole Map

17 K-band Map (23 GHz)

18 Ka-band Map (33 GHz)

19 Q-band Map (41 GHz)

20 V-band Map (61 GHz)

21 W-band Map (94 GHz)

22 Final Map

23 Comparison COBE-WMAP 53 GHz 94 GHz (30 times finer)

24 Difference Map

25 Spherical harmonics

26 Power Spectrum I T n = l l m= l a lm Y lm n C Θ T n 1 T n 2 n 1 n 2 =cos Θ l 2 l 1 Y lm n 1 Y lm n 2 = 4 π P l n 1 n 2 m= l 1 C Θ = a l2 P l cos Θ 4π l alm 2 al = 2 m

27 Power Spectrum II C l = alm m = a = a 2 l 1 m lm 2 l 1 l 2 1 C Θ = 2 l 1 C l P l cos Θ 4π l ΔT l = C l l l 1 /2 π

28 Power Spectrum III π Θ~ l

29 Primordial fluctuation region Θ 2 l l dec 90 Angular scales larger than the causal horizon size at decoupling as observed today (primordial fluctuation spectrum)

30 Acoustic Peak Region 2 > Θ l 900 This region can be described by the physics of a 3000 K plasma with a number density of ne=300 cm-3 responding to fluctuation in the gravitational potential of dark matter (acoustic peak region)

31 Silk Damping Tail Θ 0. 2 l 900 The structure is produced by the diffusion of the photons from the potential fluctuations, and the washing out of the net observed fluctuations by the large number of cold and hot regions along the line of sight (Silk damping tail)

32 Interpretation of the peaks Interpretation in terms of a flat adiabatic ΛCDM-cosmological-model Only the position of the peaks and their ratios are considered Physics of the acoustic peaks may be understood in terms of: ω b,ω m, n s, τ,θ A b h baryon density 2 m h 2 ω m =ω b ω c matter density spectral index angular scale of the sound horizon at decoupling optical depth at reionization

33 Peak ratios For l>40 the peak ratios are insensitive to the intrinsic amplitude of the power spectrum and τ due to: Scattering of free electrons from reionization (z=20) with CMB photons -> lowering the fluctuation by nearly a constant factor

34 The first acoustic peak - The peaks arise from adiabatic compression of the photon-baryon-fluid as it falls into preexisting wells in the gravitaional potential - The potential wells are the result of some primordial field fluctuation (e.g. inflation field) - The wells are enhanced by the dark matter (does not scatter off the baryons and photons) - The first peak corresponds to the scale of the mode that has compressed once in the age of the universe (the photons decoupled from the electrons, t=379 kyr after Big Bang)

35 Angular scale of the peaks comoving size of the sound horizon at decoupling r s z dec Θ A= d A z dec angular diameter distance to the decoupling surface

36 Geometric degeneracy ωm, ωb Are well measured (affect the spectrum at early times) (assumption: flat geometry) Geometric degeneracy: Same A for different ω m, ω b and h ω m = m h 2 ω b = b h 2 It can be shown that A is the same for constant m h 3. 4

37 Age of the Universe 1 limits on m isochrons Seperation of m and h b fixed to (1 region) (position of the first peak) b fixed to (2 region) (position of the first peak) 1 and 2 region of the full analysis m h 3. 4 =const Θ A t 0 =6.52 h 1 1 m 1/ 2 ln 1 1 m m [ Gyr ]

38 Basic Results Description Symbol Value Uncertainty Total density Dark energy density Baryon density Matter density Light neutrino density CMB Temperature (K) Redshift at decoupling Hubble constant Age of universe (Gyr) Age at decoupling (kyr) Age at reionization (Myr) tot < % CL (-80) b m tcmb zdec h t0 tdec m ν ev tr Standard model of cosmology: flat -dominated universe seeded by a nearly scale-invariant adiabatic Gaussian fluctuation fits the data

Future: Planck - Start in the first quarter of 2007 - Frequencies from 30 GHz to

39 Future: Planck - Start in the first quarter of Frequencies from 30 GHz to 857 GHz -Angular resolution: 5.0 arcmin to 33 arcmin (WMAP: 13.8 arcmin 55.8 arcmin)

40 References - The Cosmic Microwave Background Data and their Implications for Cosmology, V.Tudose, Romanian Reports in Physics, Volume 55, Number 2, P , First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results, C.L. Bennett et al. Astrophysical Journal - Two-Point Correlations in the COBE DMR Four-Year Anisotropy Maps, G. Hinshaw et al. Astrophysical Journal, 464:L25-L28, 1996 June 10 - First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Interpretation of the TT and TE Angular Power Spectrum Peaks, L. Page et al. Astrophysical Journal - WMAP-Homepage: - PLANCK-Homepage: - First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: The Angular Power Spectrum, G. Hinshaw et al. Astrophysical Journal - First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters

41 Angular scale of the peaks II ωγ 1 Rdec Rdec Req r s z dec =3997 ln ωm ωb 1 Req R z =3 ρ b z /4 ργ z 1 z eq = 5464 ω m / T CMB / ρ ν / ργ redshift at matter-radiation equality

42 Angular scale of the peaks III z dec d A= 0 H 1 0 dz 1 z 4 r 3 m 1 z Λ angular diameter distance to the decoupling surface for a flat geometry Λ =1 m r matter density current radiation density

43 Age of the Universe I - First acoustic peak in the CBM power spectrum: known acoustic size: r s =147±2 Mpc z dec =1089±1 at redshift: 0. 2 d =14. 0 Decoupling surface: A 0. 3 Gpc t 0 =6.52 h 1 1 m 1 m 1/ 2 Age: t 0 =13.7±0. 2 Gyr 1 ln m [ Gyr ]

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