Constraining the small-scale primordial power spectrum Donghui Jeong (Penn State) YITP cosmology seminar, 21 May 2018
Our Physical Cosmology The Universe is spatially flat , and the expansion is accelerating . • Source: NASA/WMAP science team
The concordance cosmology
Remaining big questions • From ASTRO2010 decadal review: All related to the nature of the building blocks of the concordance model: • Dark energy: Why is the Universe accelerating now? • Inflation: How did the Universe begin? • Dark matter: What is dark matter? • Neutrinos: What are the properties of neutrinos? • Seize every opportunity to leave no stone unturned!
Remaining big questions • From ASTRO2010 decadal review: All related to the nature of the building blocks of the concordance model: • Dark energy: Why is the Universe accelerating now? • Inflation: How did the Universe begin? • Dark matter: What is dark matter? • Neutrinos: What are the properties of neutrinos? • Seize every opportunity to leave no stone unturned !
Inflation questions • How did inflation begin? • What accelerated the Universe? • How did it end? • How do we connect inflation to the beginning of the hot, dense initial state of the Big-bang cosmology?
Inflation questions • How did inflation begin? • What accelerated the Universe? • How did it end? • How do we connect inflation to the beginning of the hot, dense initial state of the Big-bang cosmology?
A key to inflationary cosmology redshift z 10 8 10 6 10 4 10 2 0 10 4 10 − 4 δ ∝ a 2 δ ∝ a comoving horizon 1 / ( aH ) [Mpc/ h ] 10 3 10 − 3 500 Mpc/ h wavenumber k [ h /Mpc] 10 2 10 − 2 65.7 Mpc/ h 10 1 10 − 1 10 0 10 0 1 Mpc/ h � H quantum � 10 − 1 10 1 ∼ fluctuations δ ∝ ln a δ ∝ a 2 π 10 − 2 10 2 Inflation RD MD ? 10 − 3 10 3 10 − 8 10 − 6 10 − 4 10 − 2 1 scale factor a
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Bringmann, Scott & Akrami (2011) Constraint over the broader range
Bringmann, Scott & Akrami (2011) For secluded DM!
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For secluded DM + PBH Note: The constraint is milder as the PBH abundance scales only as erf(P δ ).
Constraint II. Thermal history Planck Collaboration
Damping of CMB power spectrum Planck Collaboration
Silk damping and Diffusion scale temperature anisotropies at ~0.0001’’ scale
Silk damping and Diffusion scale 1 mean free path: λ mfp ' σ e γ n e # of scatters: N ' σ e γ n e H − 1 diffusion scale (r.m.s. of random walk): p 1 λ D ' λ mfp N ' p σ e γ n e H temperature anisotropies at ~0.0001’’ scale
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