Big Bang, and the Cosmic Microwave Background Eiichiro Komatsu (Max-Planck-Institut für Astrophysik, Garching) Celebration for the continuation of the Universe Cluster Deutsches Museum, November 22, 2012 1
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? 2
The Breakthrough • Now we can observe the physical condition of the Universe when it was very young. 3
Cosmic Microwave Background (CMB) • Fossil light of the Big Bang! 4
From “Cosmic Voyage”
Night Sky in Optical (~0.5µm) 6
Night Sky in Microwave (~1mm) 7
Night Sky in Microwave (~1mm) T today =2.725K COBE Satellite, 1989-1993 8
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 9 Wavelength
Arno Penzias & Robert Wilson, 1965 • Isotropic • Unpolarized 10
“For their discovery of cosmic microwave background radiation” 11
P. Roll and D. Wilkinson, 1966 D.Wilkinson (W of WMAP) 12
• The spectrum of CMB has a peak at 1.1mm. Dr. Hiranya Peiris • Let’s compare it with … University College London –Microwave oven: 12cm –Cellular phone: 20cm –UHF Television: 39-64cm –FM radio: 3m –AM radio: 300m You can “see” CMB by TV (not by a cable TV of course!). Perhaps you can “hear” CMB by a cell phone? 13
How was CMB created? • When the Universe was hot, it was a hot soup made of: • Protons, electrons, and helium nuclei • Photons and neutrinos • Dark matter (DM) • DM does not do much, except for providing a a gravitational potential because ρ DM / ρ H,He ~5 14
Universe as a hot soup • Free electrons can scatter photons efficiently. • Photons cannot go very far. proton photon helium electron 15
Recombination and Decoupling • [ recombination ] When the temperature 1500K falls below 3000 K, almost all electrons are captured by protons 3000K and helium nuclei. Time • [ decoupling ] Photons are no longer scattered. I.e., photons 6000K and electrons are no longer coupled. proton electron helium photon 16
Smoot et al. (1992) COBE/DMR, 1992 1cm 6mm 3mm • 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
used to be 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: The seven-year data release • L2 is a million miles from Earth September 8, 2010: • WMAP leaves Earth, Moon, and Sun WMAP left L2 21 behind it to avoid radiation from them
used to be WMAP at Lagrange 2 (L2) Point June 2001: WMAP launched! February 2003: The first-year data release We are currently working March 2006: on the final data release! The three-year data release (nine-year data release) March 2008: The five-year data release January 2010: The seven-year data release • L2 is a million miles from Earth September 8, 2010: • WMAP leaves Earth, Moon, and Sun WMAP left L2 22 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 23 - command/data handling deployed solar array w/ web shielding - battery and power control
COBE to WMAP (x35 better resolution) COBE COBE 1989 WMAP WMAP 24 2001
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. • D.N. Spergel • D. Larson Verde • G.S. Tucker • E.L. Wright • M.R. Nolta 25
Cosmic Pie Chart: 7-year • Standard Model • H&He = 4.58 % (±0.16%) • Dark Matter = 22.9 % (±1.5%) • Dark Energy = 72.5 % (±1.6%) • H 0 =70.2±1.4 km/s/Mpc • Age of the Universe = 13.76 billion “ScienceNews” article on years (±0.11 billion years) the WMAP 7-year results How did we obtain these numbers? 26
23 GHz [unpolarized] 27
33 GHz [unpolarized] 28
41 GHz [unpolarized] 29
61 GHz [unpolarized] 30
94 GHz [unpolarized] 31
How many components? 1. CMB : T ν ~ ν 0 2. Synchrotron (electrons going around magnetic fields): T ν ~ ν –3 3. Free-free (electrons colliding with protons): T ν ~ ν –2 4. Dust (heated dust emitting thermal emission): T ν ~ ν 2 5. Spinning dust (rapidly rotating tiny dust grains): T ν ~complicated You need at least five frequencies to separate them! 32
Galaxy-cleaned Map 33
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 34 WMAP
COBE/DMR Power Spectrum Angle ~ 180 deg / l ~9 deg ~90 deg (quadrupole) 35 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 36 WMAP
WMAP Power Spectrum Angular Power Spectrum Large Scale Small Scale COBE about 1 degree on the sky 37
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 38 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) 39
CMB Polarization • CMB is (very weakly) polarized! 40
“Stokes Parameters” North East Q<0; U=0 41
23 GHz [polarized] Stokes Q Stokes U 42
23 GHz [polarized] North Stokes Q Stokes U East 43
33 GHz [polarized] Stokes Q Stokes U 44
41 GHz [polarized] Stokes Q Stokes U 45
61 GHz [polarized] Stokes Q Stokes U 46
94 GHz [polarized] Stokes Q Stokes U 47
How many components? 1. CMB : T ν ~ ν 0 2. Synchrotron (electrons going around magnetic fields): T ν ~ ν –3 3. Free-free (electrons colliding with protons): T ν ~ ν –2 4. Dust (heated dust emitting thermal emission): T ν ~ ν 2 5. Spinning dust (rapidly rotating tiny dust grains): T ν ~complicated You need at least THREE frequencies to separate them! 48
Physics of CMB Polarization Wayne Hu • CMB Polarization is created by a local temperature quadrupole anisotropy. 49
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 . 50
Radial and Tangential Polarization Patterns around Temp. Spots • All hot and cold spots are stacked • “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 51
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 52
Gravitational waves are coming toward you... What do you do? • Gravitational waves stretch space, causing particles to move. 53
Two Polarization States of GW • This is great - this will automatically generate quadrupolar anisotropy around electrons! 54
From GW to CMB Polarization Electron 55
From GW to CMB Polarization Redshift R e d s h i f t t f i h s Blueshift Blueshift e u l B t f i h s e u R l B e d s h i f t Redshift 56
From GW to CMB Polarization Gravitational waves can produce both E- and B-mode polarization 57
“Tensor-to-scalar Ratio,” r r = [Power in Gravitational Waves] / [Power in Gravitational Potential] Theory of “Cosmic Inflation” predicts r <~ 1 – I will come back to this in a moment 58
Polarization Power Spectrum • No detection of B-mode polarization yet. B-mode is the next holy grail! 59
Recommend
More recommend
