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The Planck Mission: Scientific expectations

Scientific Expectations. The Planck Mission: Scientific expectations. Lucia A. Popa. ISS I nstitute for S pace S ciences, Bucharest. Lucia Popa ISS I nstitute for S pace S ciences, Bucharest.

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The Planck Mission: Scientific expectations

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  1. Scientific Expectations The Planck Mission: Scientific expectations Lucia A. Popa ISS Institute for Space Sciences, Bucharest Lucia Popa ISSInstitute for Space Sciences, Bucharest Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  2. Planck Mission Looking back down to the time Outline Planck milestones and challenges Cosmology @ ISS Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  3. Planck home page: http://www.rsd.esa.int/index.phd?project=Planck • Third generation space CMB Mission • Primary scientific goal:measure the CMB temperaturand polarization anisotropies to fundamental limits down to 5’ • Current launch date: December 2008 together with Hershel on an Ariane 5 rocket • Schedule • Broad Science • Primary anisotropies • cosmological parameters, dark energy,inflation • Secondary anisotropies: • Gravitational lensing, reionization,galaxy clusters, • massive neutrinos • Non-CMB science • Extragalactic • Galactic The Scientific Program of Planck ESA-SCI (2005) 1 (Blue Book) arXiv:astro-ph/0604069 Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  4. Instruments Planck frequencies & Foregrounds WMAP frequencies & Foregrounds Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  5. Last scattering surface COBE: http://aether.lbl.gov/www/projects/cobe • CMB photons emerge from the photosphere at recombination • Temperature inhomogeneities at recombination become anisotropy to the observer at present • Spot sizes ranging from fraction of a degree to 180 degrees • Spots of a given angular scale gives the power spectrum • linear theory Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  6. Anisotropy Formation • Initial temperature inhomogeneities oscillate as sound waves in the plasma before recombination • T ~ 3000 K photons ionize hydrogen • Coulomb interactions + Thomson scattering: baryon-photon plasma – perfect fluid • Fluid falls into CDM potential wells : acoustic oscillations • Oscillations frozen at recombination • Compression=hot spotsRarefaction=cold spots • Hot and cold spots appear as temperature anisotropies • Spectrum of sound shows harmonics at integer ratios of the fundamental based on the distance sound travels by recombination • First peak = mode that just compresses • Second peak = mode that compresses then rarefies • • Harmonic peaks: 1:2:3 in wavenumber Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  7. Angular scales measure the angular diameter distance to recombination involving the curvature, dark energy, matter and radiation content of the Universe Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  8. more clumpy Acoustic peaks structure of the CMB power spectrum: direct confirmation of the cosmological model CDM Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  9. CMB CMB + HST CMB +HST + SN1A SN1A First acoustic peak: curvature of the Universe < 0 open = 0 flat > 0 closed direct prediction of inflation Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  10. Second acoustic peak : baryonic content of the Universe agreement with BBN prediction • baryons drag the fluid into potential wells • enhance the compressional peaks (odd) over the rarefaction peaks (even) • e.g. suppression of the second peak Third acoustic peak : Cold Dark Matter content of the Universe W. Hu ( 2007 ) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  11. Toward the Standard Cosmological Model Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  12. f=/cdm M. Tegmark (1998) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  13. Milestones: Past & Present • Large-scale anisotropy: COBE DMR 1992 • Degree-scale anisotropy many: 1993-1999 • First acoustic peak: Toco, Boom, Maxima, WMAP 1999 -2008 • Secondary acoustic peak(s): DASI, Boom 2001 • Damping tail CBI: 2002 W. Hu (2001) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  14. Measurement + Data reduction +Physical assumptions Homogeneity and Isotropy: Random Gaussian field: Anisotropy power spectrum: Cosmic Variance: Criticalities:fsky , angular resolution, sensitivity (μK/pixel) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  15. Friedmann-Robertson-Walker metric perturbation: Expansion rate: Phase-space evolution in the expanding Universe: Energy-momentum tensor Tμ: Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  16. First-order perturbed Einstein equation: photons Neutrios Λ cdm m3=0.05 eV baryons m2=0.009 eV m1≈ 0 eV Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  17. CDM standard cosmological model • CDM issues: • Dark Matter: cold, warm, hot • Nature of Dark Energy: -cosmological constant or quintessence filed • -equation of state: constant or time varying • -GR is not correct? • Primordial density perturbations generation mechanism: • Inflation or Topological Defects (strings, global monopoles, textures, etc…) • Reionization of the IGM Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  18. Planck Milestone 1: to measure the CMB temperature anisotropy power spectrum limited only by the cosmic variance out into the dampingtail. Planck has : 10 × the sensitivity of WMAP 3 × the angular resolution Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  19. Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  20. Planck Milestone 2: to measure the CMB polarization power spectrum (E-mode) up to l=1000 Limiting factors: - knowledge of polarized foregrounds at Planck frequencies - instrumental noise Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  21. Planck Milestone 3: challenge the Cosmological Standard Model - break the cosmological parameters degeneracy - Increase the precision of all cosmological parameters: high discovery potential WMAP Planck Baryon density Cold Dark Matter density Optical depth to reionization of IGM Primordial perturbations spectral index Running Primordial amplitude Hubble constant Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  22. Planck challenge 1: detection of B-mode polarization of the CMB as signature of primordial gravitational waves • Polarization is generated by Thomson scattering of the anisotropic radiation Anisotropies can be generated by: • scalar perturbation: E-mode polarization E’ (n’) = E (n) • gravitational waves: B-mode polarization B’ (n’) = B (n) • Amplitude ~ energy scale of inflation Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  23. Slow-roll inflation conditions: Inflation observables: Nature of density perturbations: • Adiabatic • Isocurvature • Mix Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  24. Present Planck r=0.1 Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  25. Planck challenge 2 Vacuum Energy Density: cosmological constant or quintessence ? Common parameterization: w=-1 Cosmological constant: Dynamical Dark Energy generated by a scalar field (cosmon): w(t) < -1 Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  26. Quintessence slows down the growth of structure Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  27. z~1100 z=0 Gravitational potential can be statistically reconstructedfrom the CMB maps CMB weak lensing Planck BPOL Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  28. fn= Ωn /Ωdm without lensing with lensing A. Lewis (2006) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  29. Lesgourgues et al. (2006) Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  30. 2 X 2 tensor T=(I11+I22)/4 Q=(I11-I22)/2 U=I12/2 Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  31. Conclusions • After Planck, we will have precise knowledge of the Universe at z 1000 • • We will have tightly constrained the physics densities of matter and baryons, the • amplitude of the fluctuations in the linear phase over three decades in length • scale, and the shape of the primordial power spectrum • • Our knowledge of physical conditions and large-scale structure at z 1000 will be • better than our knowledge of such quantities at z = 0 • • If dark energy is a “recent” phenomenon, then we can translate this knowledge • reliably to intermediate redshifts, currently at the observational frontier • • Many of the Planck achievements will be assumed as priors by future mission concepts, etc. (e.g., all JDEM concepts, Cosmic Inflation Probe, CMBPol, EUCLID)

  32. Cosmology @ ISS http://venus.nipne.ro/new1/cosmo Main Projects: Planck, SPACE Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

  33. Dark Energy European Mission ESA Cosmic Vision (2015-2025) SPACE: Spectroscopic All-sky Cosmic Explorer): near-infrared 3-D spectra of 109 galaxies • 1.5m non-cryogenic telescope • large-format infrared detectors with nearly perfect quantum efficiency • digital micro-mirrors (DMD) : reconfigurable focal plane for multi-object spectroscopy

  34. Past year publications WMP 5-year constraints on the lepton asymmetry and radiation energy density: Implications for PLANCK, Jour. Of Cosmology and Astropart. Physics, 06, 028 (2008) arXiv:0804.2971 CMB polarization constraints on radiative feedback, Monthly Notices of the Royal Astronomical Society, Volume 385, Issue 1, pp. 404-410, 2008 arXiv:07.1913 Detectable Signature of Cosmic Radiative Feedback, Monthly Notices of the Royal Astronomical Society, Volume 384, Issue 4, pp. 1525-1532, 2008 arXiv:0712.0538 Constraints on time variation of fine structure constant from WMAP-3yr data, New Astronomy, Volume 12, Issue 8, p. 635-640 arXiv:0707.0190v1 Constraints on non-thermal Dark Matter from Planck lensing extraction, Jour. of Cosmology Astropart. Phys., 10, 017 (2007) arXiv:0708.2030 PLANCK-LFI scientific goals: Implications for the reionization history, New Astronomy Rev. 51 (3-4): 298-304 (2007) The Planck LFI RCA flight model test campaign, New Astronomy Rev. 51 (3-4): 305-309 (2007) The low frequency instrument on-board the Planck satellite: Characteristics and performance, New Astronomy Rev. 51 (3-4): 287-297 (2007) Probing neutrino properties with Planck Mission, Cosmic Microwave Radiation, Aspen Center for Physics 27-Jan. – 2 Feb. 2008 Observational constraints on the lepton asymmetry and radiation endergy density, Proceedings of the Carpathian Summer School of Physics, Sinaia Aug 20-31, 2007 (edt. L. Trache, S. Stoica), American Institute of Physics Conference Proceedings Sterile Neutrino as Dark Matter candidate from CMB alone, Proceedings of Eleventh Marcel Grossmann Meeting on General Relativity, (edt. H. Kleinert,R.T. Jantzen, R. Ruffini)  World Scientific, Singapore, 2007 arXiv:astro-ph/0701331 Probing cosmic dark ages with CMB polarization measurements, Proceedings of Eleventh Marcel Grossmann Meeting on General Relativity, (edt. H. Kleinert,R.T. Jantzen and R. Ruffini)  World Scientific, Singapore, 2007 Lucia A. Popa ANTARES General Collaboration Meeting Sinaia 23 – 26 Sept. 2008

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