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Cosmic Microwave Background

Cosmic Microwave Background. Acoustic Oscillations, Angular Power Spectrum, Imaging and Implications for Cosmology. Carlo Baccigalupi, March 31, 2004. Outline…. Present: angular power Future: Imaging CMB cleaning Primordial non-Gaussianity Reionization Lensing ….

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Cosmic Microwave Background

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  1. Cosmic Microwave Background Acoustic Oscillations, Angular Power Spectrum, Imagingand Implications for Cosmology Carlo Baccigalupi, March 31, 2004

  2. Outline… • Present: angular power • Future: Imaging • CMB cleaning • Primordial non-Gaussianity • Reionization • Lensing • …

  3. The Present CMB: Measuring Angular Power

  4. Before And After The First Light

  5. From COBE to WMAP Courtesy of the NASA/WMAP Science Team

  6. WMAP Maps 23 GHz, 0.82o , 6 mK/Nobs 33 GHz, 0.62o ,3 mK/Nobs Nobs ' 103 41 GHz, 0.49o ,2 mK/Nobs 94 GHz, 0.21o , 1.4 mK/Nobs 61 GHz, 0.33o , 1.4 mK/Nobs Courtesy of the NASA/WMAP Science Team

  7. The CMB Angular Power Spctrum

  8. Throwing Pebbles In The Primordial Pond Homogeneity & Isotropy + + Black Body Spectrum + Courtesy of the NASA/WMAP Science Team

  9. The Sound Of The Early Universe Adiabatic Isocurvature

  10. +

  11. The Window On The Early Universe d T/T/dr/r 0 on all scales

  12. Cosmological Parameters Basic Analysis: h, ns, k ¢dns/dk, b h2, m h2, A,  Extension: , m ,wDE, r WMAP, WMAP+ACBAR+CBI+2dF+Lyman b h2 =0.022§ 0.001,0.0224 § 0.0009 m h2 =0.14§ 0.01,0.135 +0.008 -0.009 +0.04 h=0.71§ 0.06,0.71 -0.03  =0.20§ 0.07,0.17 § 0.06 ns=0.91§ 0.06,0.93§ 0.03 +0.016 k ¢dns/dk =...,-0.031 -0.017 +0.09 A=0.9 § 0.1,0.83 -0.08

  13. Extension:  WMAP+ACBAR+CBI+HST+SNIa+(H0>50 km/sec/Mpc): =1.02 § 0.02 Extension: m WMAP+ACBAR+CBI+2dF: h2=imi/93.5 eV < 0.0076´ m <0.23 eV Extension: wDE WMAP+ACBAR+CBI+HST+SNIa+2dF: wDE < -0.78 Extension: r WMAP+ACBAR+CBI+2dF+infl.cons.rel.: r < -0.71

  14. Reionisation ClT/ exp(-2) on l > lrh ClT,TE,E,B boosted on l < lrh ' 0.12

  15. The Future CMB: Imaging Cosmology

  16. CMB Spectrum…

  17. CMB Spectrum… Primordial Density Perts.: non-Gaussian? Reionization: Non-Gaussian Primordial GWs Lensing: Non-Gaussian

  18. CMB Spectrum…

  19. Planck According To Dodelson & Hu 2003

  20. True CMB…

  21. WMAP CMB…

  22. True CMB…

  23. Planck CMB…

  24. True CMB…

  25. CMBpol CMB…

  26. CMB Corrupted

  27. The Future CMB: Foreground Removal

  28. CMB Corrupted

  29. Fast Independent Component Analysis (FastICA) x=As+n, find W such that Wx=s+Wn FastICA main loop: construct W row by row Choose initial w Update through wnew=E[xg(wTx)]-wE(g’(wTx)) Compare with w. If not converged go back; if converged start up next row, keeping orthogonality

  30. FastICA on Planck SimulationsMaino et al. 2002 Planck nominal performance IN OUT

  31. Component Separation in Polarisation See Baccigalupi et al. 2003 for results with Planck nominal performance

  32. FastICA and COBE • Perform Monte Carlo simulations to quantify the effect of noise distribution • Build Criteria to Identify Physical Components in a Heavy Noise Enviroment • Add priors to check quality and consistency of the results • Extract Cosmological Parameters and Foreground Science Maino et al. 2003

  33. FastICA & COBE Maino et al. 2003 Blind Non-Blind

  34. The Future CMB: Imaging Physical Cosmology

  35. Primordial non-Gaussianity Y =YL+fNL(YL2-<YL2>) The simplest inflationary scenario predicts fNL' 10-1 WMAP: -58< fNL< -134 Planck forecast in progress Liguori et al. 2003

  36. Imaging Reionization… 9.5 arcminutes Normal Stars in proto-galaxies 20% escape fraction d T/T CMB scattering on moving electorns t compatible with WMAP Salvaterra, Ferrara et al. 2004 in prep.

  37. Dark Energy & CMB: beyond Cl s L f Giovi et al. 2003, PRD in press, astro-ph/0308118

  38. CMB bispectrum L Q (W ) ´dT(W )/T alm=sQ (W )Ylm(W )dW Blm l`m`l``m``=alm al`m` al``m`` Bl l`l``=åm m` m`` (mlm`l`m``l``) alm al`m` al``m`` l f l`` l`

  39. CMB bispectrum & Structure Formation L < Blm l`m`l``m`` >=0 < Blm l`m`l``m`` >0 f

  40. CMB bispectrum & Structure Formation L Q (W ) =Qlss(W +dW)+QISW 'Qlss(W)+rQlss(W)¢dW QISW(W )=2s0decdr dY (r,W )/dh dW =2s0decdr[(r-rdec)/rdecr]Y(r,W) <Bl l`l``>=[(2l+1)(2l`+1)(2l``+1)/16p]1/2(0l0l`0``l``) ¢ ¢ [l(l+1)- l`(l`+1)+ l``(l``+1) ]Cl Q(l``)+Perm. D(z)=[r(zdec)-r(z)]/r(zdec)r(z)3 f Q(l)=s0dec D(z) F(z) dz F(z)=dPY/dz|k=l/r(z) PY=(3Wm0 /2)2(H0/ck)4P(k,z)(1+z)2 P(k,z)=AknT(k,z)2 Hu & White 1997, Bartelmann & Schneider 2001, Komatsu & Spergel 2001, Verde & Spergel 2002

  41. CMB bispectrum & Structure Formation L z r l =2p /k=r(z3)/l z3 r(z3) l =r(z2)/l z2 r(z2) l =r(z1)/l f z1 r(z1) l-1

  42. L CMB bispectrum line of sight chronology z r z!1 :super-horizon scales in a flat CDM universe, dPY/dh =0, dQ/dz! 0 horizon crossing, Y decaying linearly, dQ/dz>0 onset of acceleration, change in cosmic equation of state, Y decaying linearly, dQ/dz>0 Non-linearity, Y grows, dQ/dz<0 f z! 0, l vanishes, dQ/dz! 0 l-1

  43. CMB bispectrum line of sight distribution L f Giovi et al. 2003, PRD in press, astro-ph/0308118

  44. CMB bispectrum & Dark Energy L Quintessence reference models SUGRA RP f

  45. CMB bispectrum & Dark Energy L Ma et al. 1999, Smith et al. 2003 f Giovi et al. 2003, PRD in press, astro-ph/0308118

  46. CMB bispectrum & Dark Energy L f Giovi et al. 2003, PRD in press, astro-ph/0308118

  47. CMB bispectrum & Dark Energy L f Giovi et al. 2003, PRD in press, astro-ph/0308118

  48. CMB bispectrum & Dark Energy L f Giovi et al. 2003, PRD in press, astro-ph/0308118

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