Cosmology(from(the( microwave( background( Jo(Dunkley( - - PowerPoint PPT Presentation
Cosmology(from(the( microwave( background( Jo(Dunkley( University(of(Oxford( Jo Dunkley History of early universe Inflation? T 10 15 GeV t 10 -35 s CDM decoupling? T 10 GeV? t 10 -8 s Neutrino decoupling T 1 MeV t
Inflation? T ∼ 1015 GeV t ∼ 10-35 s CDM decoupling? T ∼ 10 GeV? t ∼ 10-8 s Neutrino decoupling T ∼ 1 MeV t ∼ 1s Big Bang Nucleosynthesis T ∼ 100 keV t ∼ 10 min Matter-Radiation Equality T ∼ 0.8 eV t ∼ 60,000 yr Recombination T ∼ 0.3 eV t ∼ 380,000 yr Later: Neutrinos become ‘cold’ < t~100,000,000 yr
1. Inflation (?) imprints quantum fluctuations. 2. Space expands, regions enter into causal contact and start to evolve. 3. Coupled baryons and photons produce oscillations in plasma. After 380,000 years the fluctuations have evolved, and we see a snapshot
Linearity means we can use the anisotropies to infer the initial fluctuations and the contents of the Universe.
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Planck(Collaboration(2015
X mν < 0.68 eV More species: longer radiation domination, suppress acoustic oscillations, anisotropic stress shifts peaks More mass: neutrinos switch from being relativistic (hot) to non-relativistic (cold) earlier. Hot neutrinos free-stream, reducing matter clustering and damping of photon-baryon oscillations compared to CDM.
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