xi. the hot big bang and the cosmic microwave...
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XI. The Hot Big Bang and the Cosmic Microwave Background
ASTR378 Cosmology : XI. Hot Big Bang and CMB 143
Properties of the CMB
• The Cosmic Microwave Background (CMB) has the spectrum of a blackbody with T0 = 2.725±0.001 K
• Energy density of radiation:
ASTR378 Cosmology : XI. Hot Big Bang and CMB 144
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εγ ≡ ρradc2 = αT 4
α = π 2kB4
15h3c 3≈7.565×10-16 J m-3 K-4
Critical Density and the CMB
• At the present day, the energy density in the CMB is
which, as a fraction of
ρcrit gives Ωγ(t0)~ 5×10-5, << than Ωbary(t0)~0.04
• We know the radiation density goes as
so the Universe cools as it expands
• The spectrum of the CMB is still a blackbody, just at a lower temperature
• ρrad(t0) << ρbary(t0) ; what about the numbers of photons and baryons?
ASTR378 Cosmology : XI. Hot Big Bang and CMB 145
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εγ ≡ ρradc2 = αT 4 ≈ 4.2 × 10-14 J m-3,
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ρrad ∝1a4; ρrad ∝T
4
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T ∝ 1a
The Photon / Baryon Ratio
• If we divide the energy density of the CMB by the mean energy per photon, we get nγ(t0) ~ 4.11 × 108 m-3
• We can get the number density of baryons from Ωbary ~ 0.04 and the mass of a proton (≈ mass of a neutron) nbary(t0) ~0.22 m-3
• The ratio of baryons to photons η≈ 5 × 10-10 there are roughly two billion photons for every baryon (!)
ASTR378 Cosmology : XI. Hot Big Bang and CMB 146
ASTR378 Cosmology : XI. Hot Big Bang and CMB 147
Recap: The Origin of the CMB
• Early Universe much hotter and denser typical γenergetic enough to ionise H a “sea” of nuclei and e-
• γinteract strongly with free e- frequent collisions, short mean free path of γ Universe opaque
• As the Universe expanded and cooled, <εγ> , typical γ no longer able to ionise H γ can travel freely decoupling
ASTR378 Cosmology : XI. Hot Big Bang and CMB 148
Recap: The Surface of Last Scattering
• Decoupling occurred when the Universe was ~ 3000 K, before then in a highly-interacting thermal state uniform (to ~10-5) BB spectrum in all directions (steady state theory)
• CMB photons come from when the Universe was ~1100× smaller, and originate from a sphere surface of last scattering (more like a layer...)
Schematic View of the History of the Universe ASTR378 Cosmology : XI. Hot Big Bang and CMB 149
CMB Temperature Fluctuations
• COBE spacecraft (1990’s): – to 1st order, the CMB is uniform – the CMB dipole, resulting from motion of
the satellite relative to the CMB (Earth – Sun, Sun – Galaxy, etc.)
– Once you subtract out the dipole and foreground emission from the Milky Way, you get:
ASTR378 Cosmology : XI. Hot Big Bang and CMB 150
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T = 14π
T θ,φ( )∫ sinθ dθ dφ = 2.725Κ
δTT
θ,φ( ) ≡ T θ,φ( ) − TT
; δTT
⎛ ⎝ ⎜
⎞ ⎠ ⎟ 2 1/ 2
≈1.1×10−5
COBE and WMAP
ASTR378 Cosmology : XI. Hot Big Bang and CMB 151
COBE (1990’s) WMAP (2000’s)
The Scale of CMB Temperature Fluctuations
• Can express δT/T in terms of spherical harmonics:
• Correlation function of δT/T:
• Cl measures temperature fluctuations on an angular scale θ~180°/l (l = 0: monopole, l = 1: dipole, l ≥ 2: cosmologically interesting)
ASTR378 Cosmology : XI. Hot Big Bang and CMB 152
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δTT
θ,φ( ) = almYlm θ,φ( )m=− l
l
∑l= 0
∞
∑
�
C θ( ) = 14π
(2l +1)Cll= 0
∞
∑ Pl cosθ( )
The Causes of CMB Temperature Fluctuations
• Different origins for large-scale (l < 180) and small-scale (l> 180) fluctuations
• Large-scale fluctuations: inhomogeneities in dark matter distribution affect energy of photons Sachs-Wolfe effect
• Small-scale fluctuations: acoustic oscillations of photon-baryon fluid, peak in ΔT depends on curvature
ASTR378 Cosmology : XI. Hot Big Bang and CMB 153
ΛCDM Cosmology
• Current observational constraints on Ωmat and ΩΛ from three different sources: – Type Ia supernovae (SNe, blue) – Sound waves in the Cosmic Microwave
Background (CMB, orange) – Large-scale structure in the distribution of
galaxies (Baryon Acoustic Oscillations=BAO, green)
• They all overlap at the same location • They all overlap where Ωmat + ΩΛ≈ 1;
best guess Ωmat ~ 0.3, ΩΛ~ 0.7
ASTR378 Cosmology : XI. Hot Big Bang and CMB 154
From Kowalski et al. 2008
Contours:68.3%, 95.4% and 99.7% confidence levels
k > 0
k < 0