The 7 -Year WMAP Observations: Cosmological Interpretation Eiichiro Komatsu (Texas Cosmology Center, UT Austin) Physics Colloquium, Texas Tech University, April 22, 2010 1
Cosmology: The Questions • How much do we understand our Universe? 2
Cosmology: The Questions • How much do we understand our Universe? • How old is it? 3
Cosmology: The Questions • How much do we understand our Universe? • How old is it? • How big is it? 4
Cosmology: The Questions • How much do we understand our Universe? • How old is it? • How big is it? • What shape does it take? 5
Cosmology: The Questions • How much do we understand our Universe? • How old is it? • How big is it? • What shape does it take? • What is it made of? 6
Cosmology: The Questions • How much do we understand our Universe? • How old is it? • How big is it? • What shape does it take? • What is it made of? • How did it begin? 7
The Breakthrough • Now we can observe the physical condition of the Universe when it was very young. 8
Cosmic Microwave Background (CMB) • Fossil light of the Big Bang! 9
From “Cosmic Voyage”
Night Sky in Optical (~0.5µm) 11
Night Sky in Microwave (~1mm) 12
Night Sky in Microwave (~1mm) T today =2.725K COBE Satellite, 1989-1993 13
4K Black-body 2.725K Black-body 2K Black-body Brightness, W/m 2 /sr/Hz Rocket (COBRA) Satellite (COBE/FIRAS) CN Rotational Transition Ground-based Balloon-borne Satellite (COBE/DMR) Spectrum of CMB (from Samtleben et al. 2007) 3m 30cm 3mm 0.3mm 14 Wavelength
Arno Penzias & Robert Wilson, 1965 • Isotropic • Unpolarized 15
“For their discovery of cosmic microwave background radition” 16
Smoot et al. (1992) COBE/DMR, 1992 • Isotropic? • CMB is anisotropic! (at the 1/100,000 level) 18
“For their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation” 19
CMB: The Farthest and Oldest Light That We Can Ever Hope To Observe Directly • When the Universe was 3000K (~380,000 years after the Big Bang), electrons and protons were combined to form neutral hydrogen. 20
WMAP at Lagrange 2 (L2) Point June 2001: WMAP launched! February 2003: The first-year data release March 2006: The three-year data release March 2008: The five-year data release January 2010: • L2 is a million miles from Earth The seven-year • WMAP leaves Earth, Moon, and Sun data release 21 behind it to avoid radiation from them
WMAP Spacecraft Spacecraft WMAP Radiative Cooling: No Cryogenic System upper omni antenna back to back line of sight Gregorian optics, 1.4 x 1.6 m primaries 60K passive thermal radiator focal plane assembly feed horns secondary reflectors 90K thermally isolated instrument cylinder 300K warm spacecraft with: medium gain antennae - instrument electronics - attitude control/propulsion 22 - command/data handling deployed solar array w/ web shielding - battery and power control
COBE to WMAP (x35 better resolution) COBE COBE 1989 WMAP WMAP 23 2001
WMAP First Year Science Team Principal Investigator: Charles L. Bennett Father of the CMB experiment, David Wilkinson •WMAP is currently planned to complete 9 years of full-sky survey, ending its mission in ~2010–2011. 24
WMAP 7-Year Science Team • M.R. Greason • K.M. Smith • C.L. Bennett • J. L.Weiland • M. Halpern • C. Barnes • G. Hinshaw • E.Wollack • R.S. Hill • R. Bean • N. Jarosik • J. Dunkley • A. Kogut • O. Dore • S.S. Meyer • B. Gold • M. Limon • H.V. Peiris • L. Page • E. Komatsu • N. Odegard • L. Verde • D.N. Spergel • D. Larson • G.S. Tucker • E.L. Wright • M.R. Nolta 25
WMAP 7-Year Papers • Jarosik et al. , “ Sky Maps, Systematic Errors, and Basic Results ” arXiv:1001.4744 • Gold et al. , “ Galactic Foreground Emission ” arXiv:1001.4555 • Weiland et al. , “ Planets and Celestial Calibration Sources ” arXiv:1001.4731 • Bennett et al. , “ Are There CMB Anomalies? ” arXiv:1001.4758 • Larson et al. , “ Power Spectra and WMAP-Derived Parameters ” arXiv:1001.4635 • Komatsu et al ., “ Cosmological Interpretation ” arXiv:1001.4538 26
Cosmology Update: 7-year • Standard Model • H&He = 4.56% (±0.16%) • Dark Matter = 27.2% (±1.6%) • Dark Energy = 72.8% (±1.6%) • H 0 =70.4±1.4 km/s/Mpc • Age of the Universe = 13.75 billion years (±0.11 billion years) “ScienceNews” article on the WMAP 7-year results How did we obtain these numbers? 27
Temperature Anisotropy (Unpolarized) 22GHz 33GHz 61GHz 94GHz 41GHz 28
Galaxy-cleaned Map 29
Analysis: 2-point Correlation θ •C( θ )=(1/4 π ) ∑ (2l+1) C l P l (cos θ ) • How are temperatures on two points on the sky, separated by θ , COBE are correlated? • “Power Spectrum,” C l – How much fluctuation power do we have at a given angular scale? – l~180 degrees / θ 30 WMAP
COBE/DMR Power Spectrum Angle ~ 180 deg / l ~9 deg ~90 deg (quadrupole) 31 Angular Wavenumber, l
COBE To WMAP θ •COBE is unable to resolve the structures below ~7 degrees COBE •WMAP’s resolving power is 35 times better than COBE. •What did WMAP see? θ 32 WMAP
WMAP Power Spectrum Angular Power Spectrum Large Scale Small Scale COBE about 1 degree on the sky 33
The Cosmic Sound Wave • “The Universe as a Miso soup” • Main Ingredients: protons, helium nuclei, electrons, photons • We measure the composition of the Universe by 34 analyzing the wave form of the cosmic sound waves.
CMB to Baryon & Dark Matter Baryon Density ( Ω b ) Total Matter Density ( Ω m ) =Baryon+Dark Matter • 1-to-2: baryon-to-photon ratio • 1-to-3: matter-to-radiation ratio (z EQ : equality redshift) 35
Determining Baryon Density From C l 36
Determining Dark Matter Density From C l 0.09 0.49 37
Detection of Primordial Helium (Temperature Fluctuation) 2 38 =180 deg/ θ
Effect of helium on C lTT • We measure the baryon number density, n b , from the 1st- to-2nd peak ratio. • As helium recombined at z~1800, there were fewer electrons at the decoupling epoch (z=1090): n e =(1–Y p )n b . • More helium = Fewer electrons = Longer photon mean free path 1/( σ T n e ) = Enhanced damping • Y p = 0.33 ± 0.08 (68%CL) • Consistent with the standard value from the Big Bang nucleosynthesis theory: Y P =0.24. 39
Another “3rd peak science”: Number of Relativistic Species N eff =4.3 ±0.9 from external data 40 from 3rd peak
And, the mass of neutrinos • WMAP data combined with the local measurement of the expansion rate (H 0 ), we get ∑ m ν <0.6 eV (95%CL) 41
CMB Polarization • CMB is (very weakly) polarized! 42
Physics of CMB Polarization Wayne Hu • CMB Polarization is created by a local temperature quadrupole anisotropy. 43
Principle North Hot Cold Cold Hot East • Polarization direction is parallel to “hot.” • This is the so-called “E-mode” polarization. 44
CMB Polarization on Large Angular Scales (>2 deg) Matter Density Potential Δ T/T = (Newton’s Gravitation Potential)/3 Δ T Polarization • How does the photon-baryon plasma move? 45
CMB Polarization Tells Us How Plasma Moves at z=1090 Zaldarriaga & Harari (1995) Matter Density Potential Δ T/T = (Newton’s Gravitation Potential)/3 Δ T Polarization • Plasma falling into the gravitational potential well = Radial polarization pattern 46
Quadrupole From Velocity Gradient (Large Scale) Sachs-Wolfe: Δ T/T= Φ /3 Δ T Stuff flowing in Potential Φ Acceleration a =– ∂Φ a >0 =0 Velocity Velocity gradient Velocity in the rest The left electron sees colder e – e – frame of electron photons along the plane wave Polarization Radial None 47
Quadrupole From Velocity Gradient (Small Scale) Compression increases Δ T temperature Stuff flowing in Potential Φ Acceleration Pressure gradient slows a =– ∂Φ – ∂ P down the flow a >0 <0 Velocity Velocity gradient Velocity in the rest e – e – frame of electron Polarization Radial Tangential 48
Stacking Analysis • Stack polarization images around temperature hot and cold spots. • Outside of the Galaxy mask (not shown), there are 12387 hot spots and 12628 cold spots . 49
Two-dimensional View • All hot and cold spots are stacked (the threshold peak height, Δ T/ σ , is zero) • “Compression phase” at θ =1.2 deg and “slow-down phase” at θ =0.6 deg are predicted to be there and we observe them! • The overall significance level: 8 σ 50
E-mode and B-mode • Gravitational potential can generate the E- mode polarization, but not B-modes. • Gravitational waves can generate both E- and B-modes! E mode B mode 51
E-mode Potential Φ ( k , x )=cos( kx ) Direction of a plane wave Polarization Direction • E-mode : the polarization directions are either parallel or tangential to the direction of the plane wave perturbation. 52
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