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MATTEO VIEL

STRUCTURE FORMATION. MATTEO VIEL. INAF and INFN Trieste. SISSA LECTURE nr 5 - 24 th March 2010. OUTLINE: LECTURES. Structure formation: tools and the high redshift universe The dark ages and the universe at 21cm IGM cosmology at z=2=6 IGM astrophysics at z=2-6

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MATTEO VIEL

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  1. STRUCTURE FORMATION MATTEO VIEL INAF and INFN Trieste SISSA LECTURE nr 5 - 24th March 2010

  2. OUTLINE: LECTURES • Structure formation: tools and the high redshift universe • The dark ages and the universe at 21cm • IGM cosmology at z=2=6 • IGM astrophysics at z=2-6 • 5. Cosmological probes LCDM scenario • 6. Review of main concepts

  3. OUTLINE: LECTURE 5 Lyman-a forest and weak gravitational lensing Further cosmological probes…. High redshift QSOs

  4. LY-a and WEAK LENSING

  5. Weak Lensing: Basics q b h Amplification Matrix e.g. Gunn 1967 (Feynman 1964) Van Waerbeke, Mellier 2004 (review) Complex shear g=g1 + ig2

  6. Weak Lensing: Basics - I

  7. Weak Lensing: Basics - II

  8. Weak Lensing – the COSMOS survey - I 2 sq degree 234500 sources stars, galaxies, hot gas Massey et al., 2007, Nature, 445, 286

  9. Weak Lensing – the COSMOS survey - II Cosmology (crucial to model non linear corrections!) Massey et al., 2007

  10. Weak Lensing – the COSMOS survey - III z = 0.1 – 1 z = 1 – 1.4 z = 1.4 -3 Massey et al., 2007, arXiv: astro-ph/0701480

  11. Weak Lensing and Lyman-a - I WL banana Lesgourgues, Viel, Haehnelt, Massey, 2007

  12. CFHTLS - I Canada Franca Hawaii Telescope Legacy Survey 5 bands to get photometric red. 54 sq degrees Fu et al. 2008, A&A, 479, 9

  13. Alan Heavens’s talk @ GGI

  14. WEAK LENSING PERSPECTIVES

  15. FURTHER COSMOLOGICAL PROBES

  16. Martin White lectures

  17. Cosmological parameters from baryonic oscillations Baryonic acoustic oscillation in SDSS galaxy power spectrum detected in Dec 2004 46748 LRG in 0.72 (Gpc/h)3 at <z>=0.35 - Eisenstein et al., 2005, ApJ, 633,560 - They are a standard ruler and a signature of the photons-baryons interaction in the the plasma at recombination (z=1100) and provide measurement of H (z) and DA (z) - These soundwaves could either be seen in the CMB peaks or in the galaxy powerspec. with the complication of: bias (galaxy-matter) and peculiar velocities Physical length depends on the sound horizon at recombination DM is angular diameter distance - from CMB DV = [DM2 cz/H(z)] 1/3 distance - from LRG dilation scale of the correlation function Different Wm h2

  18. Cosmological parameters from galaxy clustering Tegmark et al. 2006, PRD, in press Blake et al. 2006, MNRAS in press Padmanabhan et al. 2006, MNRAS in press Volume of SDSS LRG is 6 times The volume of the SDSS main And 10 times larger than 2dfGRS (D Pg/Pg)2 scales by the same amount

  19. Cosmological parameters from supernovae Distance modulus = m - M Dark energy in the dark ages is unconstrained Quadratic evolution linear evolution Riess et al, 2007, ApJ, 656, 451 ?

  20. Cosmological parameters from growth factors LCDM value Nesseris & Perivolaporus 2008

  21. Cosmological parameters GRBs - I Schaefer et al. 2007 Luminosity has to be estimated from the GRB spectrum Luminosity indicator vs Luminosity (this relation depends on cosmology) Examples…. GRBs tests should fit at the same time correlations and cosmology !

  22. Cosmological parameters GRBs - II Schaefer et al. 2007

  23. Sinergies Sinergies are fundamental to see if the model gives a consistent picture at different scales and z

  24. MCMC-I Estimating the likelihood of different cosmological data sets in the multidimensional parameter space is not trivial a small to map the region near The minimum well

  25. MCMC-II

  26. Inflation - I In slow roll inflation….

  27. Inflation through P(k) and Dark Energy - II P(k) depends on r, n and Running of the spectral Index dn/dlnk That describe its shape Efstathiou & Mack 2005 w = T-V/(T+V)  -1 T: kinetic energy of the scalar field V: potential energy of the scalar field Tegmark et al. 2006

  28. Lyman-alpha forest and CMB - III TENSOR TO SCALAR RATIO V=f4 Signature of gravitational waves (tensors) And inflation r V=f2 n, r and dn/dlnk are related to the inflaton potential and its derivatives n • mn (eV) < 0.68 (95 %C.L.) r < 0.55 (95 % C.L.) running = -0.055 ±0.03 WMAP3 only Seljak, Slosar. McDonald, 2006, JCAP, 0610, 014

  29. HIGH-z DARK ENERGY

  30. EARLY DARK ENERGY - I Grossi & Springel 08

  31. EARLY DARK ENERGY - II Xia & Viel 2009

  32. EARLY DARK ENERGY - III Xia & Viel 2009

  33. HIGH-z QSOs and REIONIZATION

  34. High-z QSOs-I Fan, Carilli, Keating, ARAA, 2006,44,415

  35. High-z QSOs-II

  36. High-z QSOs-III

  37. High-z QSOs-IV

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