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Additional Neutrino(s) and CMB Damping Tail

Additional Neutrino(s) and CMB Damping Tail. The timeline of the Universe. Inflation. BBN. recombination. accelerated expansion. reionization. structure formation. Legend of Λ CDM. adiabatic, nearly scale invariant, power law, Gaussian fluctuations. +. +. flatness.

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Additional Neutrino(s) and CMB Damping Tail

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  1. Additional Neutrino(s) andCMB Damping Tail 清华大学

  2. The timeline of the Universe Inflation BBN recombination accelerated expansion reionization structure formation 清华大学

  3. Legend of ΛCDM adiabatic, nearly scale invariant, power law, Gaussian fluctuations + + flatness 清华大学

  4. Cosmic Microwave Background (CMB) 清华大学

  5. Cosmic Microwave Background 1964, Penzias & Wilson 1992, COBE DMR 2010, WMAP 7yr 1990, COBE FIRAS 清华大学

  6. Ongoing high resolution CMB observations Atacama Cosmology Telescope (ACT) South Pole Telescope (SPT) PLANCK 清华大学

  7. Pushing resolution and sensitivity to new limits Credit to Sudeep Das 清华大学

  8. High resolution and sensitivity on CMB power spectrum Keisler et al., 2011, in preparation 清华大学

  9. Extra-galactic foreground components Dunkley et al., 2010 清华大学

  10. Higher resolution CMB observations are opening windows on all these epochs Inflation BBN structure formation accelerated expansion • Higher order peaks in the CMB: • Tilt and running of the primordial power spectrum • Ratio of tensor/scalar modes (r) • Primordial Helium fraction (Yp) • Number of relativistic species (Neff) • Gravitational lensing of the CMB: • Total mass of neutrinos • Growth of the structure • Dark energy behavior with redshift • Geometry of the Universe 清华大学

  11. Higher resolution CMB observations are opening windows on all these epochs Inflation BBN structure formation accelerated expansion • Higher order peaks in the CMB: • Tilt and running of the primordial power spectrum • Ratio of tensor/scalar modes (r) • Primordial Helium fraction (Yp) • Number of relativistic species (Neff) • Gravitational lensing of the CMB: • Total mass of neutrinos • Growth of the structure • Dark energy behavior with redshift • Geometry of the Universe 清华大学

  12. Less fluctuation power at small angular scales Dunkley et al., 2010 BBN consistency: 清华大学

  13. Less fluctuation power at small angular scales Keisler et al., 2011 BBN consistency: 清华大学

  14. Degeneracy between and 清华大学

  15. Primordial He abundance measurement in extra-galactic H II region Aver, Olive, Skillman, JCAP, 2011, 3, 43 Izotov, Thuan, ApJL, 2010, 710, 67 清华大学

  16. Neff explanation • Previous incorrect explanation penetrating to later papers • Increasing reduces fluctuation power at small angular scales due to the impact of the mean neutrino energy density on the expansion rate prior to/during recombination • Helium mass fraction for BBN consistency 清华大学

  17. CMB and component densities in the standard cosmological model Credit to Hu & Dodelson No baryon Baryon loading 清华大学

  18. CMB and component densities in the standard cosmological model • Co-moving Hubble radius at matter-radiation equality Credit to Hu & Dodelson 清华大学

  19. CMB and component densities in the standard cosmological model The scale of the acoustic peaks are quite sensitive to the angular scale of sound horizon 清华大学

  20. The effect of neutrino species (l>200) fixed 清华大学

  21. Diffusion (damping) length / scale Modes with λ < rdare suppressed (damped). Dependence on DA has been dropped out. 清华大学

  22. and CMB damping tail fixed fixed is computed to keep fixed Hou et al, 2011 清华大学

  23. Current constraints on Neff Vikhlinin et al., 2009, from X-ray cluster abundances at 98.4% C.L. Hou et al., 2011 Keisler et al., 2011 清华大学

  24. What if ? • WMAP7 + SPT + BAO + H0: • Transition from relativistic particles to non-relativistic ones? • PLANCK forecast 清华大学

  25. Summary • affects the fluctuation power at small angular scales due to the impact of the mean neutrino energy density on the expansion rate prior to/during recombination • characterizes the features of the damping tail in CMB power spectrum • Degeneracy direction between and • New constraints on and Planck forecast • ? 清华大学

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