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Dark energy I : Observational constraints

Dark energy I : Observational constraints. Shinji Tsujikawa (Tokyo University of Science). Dark energy. From the observations of SN Ia, CMB, and BAO etc, about 70 % of the energy density of the Universe is dark energy responsible for cosmic acceleration.

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Dark energy I : Observational constraints

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  1. Dark energy I :Observational constraints Shinji Tsujikawa (Tokyo University of Science)

  2. Dark energy From the observations of SN Ia, CMB, and BAO etc, about 70 % of the energy density of the Universe is dark energy responsible for cosmic acceleration.

  3. Observational constraints on dark energy The properties of dark energy can be constrained by a number of observations: • Supernovae type Ia (SN Ia) • 2. Cosmic Microwave Background (CMB) • Baryon Acoustic Oscillations (BAO) 4. Large-scale structure (LSS) • Weak lensing The cosmic expansion history is constrained. The evolution of matter perturbations is constrained. This is especially important for modified gravity models.

  4. Supernovae Ia observations The luminosity distance L : Absolute lumonisity s F :Observed flux is related with the Hubble parameter H, as for the flat Universe (K=0) The absolute magnitude M of SN Ia is related with the observed apparent magnitude m, via

  5. Luminosity distance in the flat Universe ______

  6. Luminosity distance with/without dark energy Flat Universe with dark energy Open Universe without dark energy Flat Universe without dark energy

  7. Perlmutter et al, Riess et al (1998) A. Riess B. Schmidt (Head of Perlmutter et al group) Perlmutter et al showed that the cosmological constant ( ) is present at the 99 % confidence level, with the matter density parameter High-z data (Perlmutter et al, 1998) The rest is dark energy.

  8. Observational constraints on the dark energy equation of state for constant w (Kowalski et al, 2008) DE SN Ia data only

  9. Time-varying dark energy equation of state

  10. Parametrization of the dark energy equation of state where

  11. Observational constraints using the parametrization Best-fit case Komatsu et al (2010) Zhao et al (2007) (SNIa, WMAP, SDSS)

  12. Observational constraints from CMB The observations of CMB temperature anisotropies can also place constraints on dark energy. 2012 PLANCK data will be released.

  13. CMB temperature anisotropies Dark energy affects the CMB anisotropies in two ways. 1. Shift of the peak position 2. Integrated Sachs Wolfe (ISW) effect ISW effect Shift for (Important for large scales) Larger Smaller scales

  14. Angular diameter distance The angular diameter distance is (flat Universe) (duality relation)

  15. Causal mechanism for the generation of perturbations Physical wavelength After the perturbations leave the Hubble radius during inflation, the curvature perturbations remain constant by the second Hubble radius crossing. Second Hubble radius crossing Scale-invariant CMB spectra on large scales Hubble radius After the perturbations enter the Hubble radius, they start to oscillate as a sound wave.

  16. CMB acoustic peaks Hu Sugiyama where

  17. where (CMB shift parameter) and

  18. The WMAP 7-yr bound:

  19. Observational constraints on the dark energy equation of state (Komatsu et al, WMAP 7-yr) Flat Universe

  20. Joint data analysis of SN Ia + CMB (for constant w ) DE The constraints from SN Ia and CMB are almost orthogonal. DE (0) (Kowalski et al, 2008)

  21. ISW effect on CMB anisotropies

  22. Evolution of matter density perturbations ) ( The growing mode solution is Responsible for large-scale structure Perturbations do not grow. The growing mode solution is

  23. Poisson equation The Poisson equation is given by (i) During the matter era (no ISW effect) (ii) During the dark energy era

  24. Usually the constraint coming from the ISW effect is not so tight compared to that from the CMB shift parameter. (apart from some modified gravity models) ISW effect

  25. CMB lensing The Atacama Cosmology telescope found the observational evidence of w = -1 dark energy from the CMB data alone by using the new CMB lensing data (2011). The lensing deflection spectrum is

  26. Baryon Acoustic Oscillations (BAO) Baryons are tightly coupled to photons before the decoupling. The oscillations of sound waves should be imprinted in the baryon perturbations as well as the CMB anisotropies. In 2005 Eisenstein et al found a peak of acoustic oscillations in the large scale correlation function at

  27. BAO distance measure The sound horizon at which baryons were released from the Compton drag of photons determines the location of BAO: We introduce (orthogonal to the line of sight) (the oscillations along the line of sight) The spherically averaged spectrum is

  28. We introduce the relative BAO distance where The observational constraint by Eisenstein et al is The case (i) is favored.

  29. Observational constraints on the dark energy equation of state from the joint data analysis of SN Ia + CMB + BAO Kowalski et al

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