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Planck 's Main Results

Planck 's Main Results. Carlos Hernández- Monteagudo Centro de Estudios de Física del Cosmos de Aragón (CE F CA), Teruel , Spain On behalf of the Planck collaboration. Outline. Introduction: CMB intensity and polarisation anisotropies. Context of Planck observations

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Planck 's Main Results

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  1. CosmoRenata meeting, Valencia, June 3rd 2013

  2. Planck's Main Results Carlos Hernández-Monteagudo Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Teruel, Spain On behalf of the Planck collaboration

  3. Outline • Introduction: CMB intensity and polarisation anisotropies. Context of Planck observations • Planck frequency maps. Computation of angular power spectra. Systematic tests. • Lensing of the CMB. Correlation to matter probes. Cosmological constraints. • Planck and other data sets. Cosmological constraints CosmoRenata meeting, Valencia, June 3rd 2013

  4. One slide on CMB angular anisotropies … In the hot, dense, ionized universe, just before hydrogen recombination, matter and radiation are in thermal EQ. (black body spectrum) and radiation pressure induced by Thomson scattering competes with gravitational attraction in slightly overdense regions, creating an acoustic oscillation pattern both in CMB photon intensity and polarization Ya.B.Zel’dovich R.A.Sunyaev Materia Radiación # of cold/hot spots in the CMB From W.Hu (1998) Gravitational potential well size 1/ Spot angular size CosmoRenata meeting, Valencia, June 3rd 2013

  5. THE OVERALL PICTURE: CosmoRenata meeting, Valencia, June 3rd 2013

  6. PLANCK VERSUS WMAP • 5 different channels at 22, 33, 44, 63, 94 GHz • Maximum angular resolution of ~0.23 degrees • Max. sensitivity of ~5 muK per square degree (94 GHz) • 10 different channels at 30, 44, 70, 100, 143, 217, 353, 545 and 857 GHz • Maximum angular resolution of ~0.075 degrees • Max. sensitivity of ~0.25 muK per square degree (143 GHz) OLD SLIDE !! • PLANCK, with many more frequency channels and better angular resolution, should: • Improve CMB measurements to smaller angular scales • Remove more efficiently the contaminants (mostly due to the Milky Way or point sources)‏ • Characterize secondary effects much more accurately • Map the E mode of the polarization to much better precision and smaller angular scales • Set constraints on the amount of B-mode polarization • Establish stronger constraints on primordial non-Gaussianity • Provide much more complete tSZ source catalog • Etc ... All this should translate into better precision in the cosmological parameters... CosmoRenata meeting, Valencia, June 3rd 2013

  7. WMAP 5 bands K band (23 GHz) Ka band (30 GHz) Q band (41 GHz) V band (61 GHz) W band (94 GHz) CosmoRenata meeting, Valencia, June 3rd 2013

  8. PLANCK 9 BANDS “Cosmological channels” Galactic and extra-galactic (Cosmic Infrared emission) dust emission CosmoRenata meeting, Valencia, June 3rd 2013

  9. Planck 4 algorithms for clean map production CosmoRenata meeting, Valencia, June 3rd 2013

  10. MAP COMPARISON(S) CosmoRenata meeting, Valencia, June 3rd 2013

  11. MAP COMPARISON(S) CosmoRenata meeting, Valencia, June 3rd 2013

  12. The angular power spectrum WMAP 7th year CosmoRenata meeting, Valencia, June 3rd 2013

  13. The angular power spectrum Planck CosmoRenata meeting, Valencia, June 3rd 2013

  14. How Planck got there … • Two different elleregimes: l < 50 and l \in [50,1500] • l<50: Gibbs sampling on all Planck channels • l>50: Two different likelihood estimators: CamSpec& Plik, using cosmological channels only [100, 143 and 217 GHz] • CamSpec is more accurate and CPU demanding. • Plikdoes not account for C_lcorrelation so accurately, but still very useful for running consistency tests • Systematic test at two levels: • Intra-pair level (pair of frequencies, after combining different subsets of detectors belonging to same frequency pair ) – probing issues like detector calibration, beam and noise characterisation • Inter-pair level (involving detectors of different frequencies) – probing foreground related issues CosmoRenata meeting, Valencia, June 3rd 2013

  15. Getting rid of galactic dust … Use 857 GHz as template for galactic dust + CIB template (derived from data) + theoretically motivated templates for Poisson, clustered, tSZ & kSZ Contribution from the Cosmic Infrared Background (CIB) Anisotropic, galactic signal! CosmoRenata meeting, Valencia, June 3rd 2013

  16. CamSpec channel pairs … CosmoRenata meeting, Valencia, June 3rd 2013

  17. CamspecVS Plick CosmoRenata meeting, Valencia, June 3rd 2013

  18. CamspecVS Plick (II) CosmoRenata meeting, Valencia, June 3rd 2013

  19. CamspecVS Plick (III) CosmoRenata meeting, Valencia, June 3rd 2013

  20. More consistency tests: 4 clean maps CosmoRenata meeting, Valencia, June 3rd 2013

  21. The low elle part … (Commander) (slight power defect at l~20, see Vielva’s talk!) CosmoRenata meeting, Valencia, June 3rd 2013

  22. The Final angular power spectrum Planck vs other exps. CosmoRenata meeting, Valencia, June 3rd 2013

  23. The angular power spectrum The case of polarization: CosmoRenata meeting, Valencia, June 3rd 2013

  24. Basic LCDM cosmological parameter set CosmoRenata meeting, Valencia, June 3rd 2013

  25. Strong limits on NG Very Gaussian universe, no hint for non Gaussianityafter correcting for the coupling of the lensing with the ISW … A lot of inflationary models ruled out … See Vielva’s talk! CosmoRenata meeting, Valencia, June 3rd 2013

  26. Cosmological parameter set The case of H0 : some tension with direct estimates of Hubble constant CosmoRenata meeting, Valencia, June 3rd 2013

  27. LCDM PARAMETER COMPARISON From http://lambda.gsfc.nasa.gov CosmoRenata meeting, Valencia, June 3rd 2013

  28. There is a lot of secondary Science … Secondary anisotropies == Anisotropies introduced along the CMB photon’s way to us by gravitational potential wells, scattering with electrons, etc • Firm detection of lensing of CMB temperature anisotropies • Firm detection of the correlation of CMB lensing to high-z, dusty sources spanning the redshift range z \in [1,5] • Detection of clusters by means of the thermal SunyaevZel’dovich effect CosmoRenata meeting, Valencia, June 3rd 2013

  29. CMB Lensing CMB light rays become deflected by the matter distribution along the line of sight by typically 2—3 arcmins. The 2D potential field generating this deflection has been detected, and its angular power spectrum measured with unprecedented accuracy: CosmoRenata meeting, Valencia, June 3rd 2013

  30. CMB Lensing (II) (Left) Simulated 2D potential field reconstruction (Below) Real 2D potential field reconstruction CosmoRenata meeting, Valencia, June 3rd 2013

  31. CMB Lensing (III) (Left) Good consistency between different measurements of potential power spectrum (Below) Measured lensing power spectrum has its own preferences wrt neutrino mass and other cosmological parameters … CosmoRenata meeting, Valencia, June 3rd 2013

  32. CMB Lensingx CIB from HFI CMB T and lensing is correlated to CIB sources at z \in [2,5] The Cosmic Infrared Background (CIB) is generated by high-z dusty galaxies and can be probed with the 545 and 857 GHz Planck channels CosmoRenata meeting, Valencia, June 3rd 2013

  33. CMB Lensingx galaxy surveys CMB Tlensingis correlated to LSS surveys sources at z \in [2,5] CosmoRenata meeting, Valencia, June 3rd 2013

  34. Planck identifies clusters via the tSZeffect … • If however the CMB encounters a hot electron plasma, then there is a net transfer of energy from the hot electrons to the cold photons. As a result, we have fewercold low energy photons and more hot high frequency photons. This results in a distortion of the black body CMB spectrum, i.e., in frequency dependent brightness temperature fluctuations. Thermal Sunyaev-Zel'dovich effect (tSZ)‏ The symbol y is known as the Comptonization parameter CosmoRenata meeting, Valencia, June 3rd 2013

  35. Catalogue of >1,227 SZ Galaxy Clusters New thermal Sunyaev-Zel’dovich clusters are mostly nearby, massive objects that are un-relaxed and hence with low X-ray emission CosmoRenata meeting, Valencia, June 3rd 2013

  36. And in combination with other data … CosmoRenata meeting, Valencia, June 3rd 2013

  37. And in combination with other data (II)… Lensing in TT angular power spectrum sets stronger constraints on neutrino masses But Lensing in its power spectrum favours massive neutrinos … ??? CosmoRenata meeting, Valencia, June 3rd 2013

  38. And in combination with other data (III)… Expected value of Neff~ 3.046, but current data favours it only for a little When included in H0 test, it alleviates tension between local Hubble estimates and estimates from the CMB CosmoRenata meeting, Valencia, June 3rd 2013

  39. Conclusions • Simple 6-parameters LCDM model fits Planck data beautifully. • Strong consistency and systematic tests. Better understanding of contaminants • Temporary polarization data largely compatible with TT (temperature) best fit model. Coherent picture. • Strong constraints on non-Gaussianity (Vielva’s talk). Presence of anomalies • Detection of CMB lensing: moderate z – universe very well described by model based upon observations at z~1,100 !! • Detection of clusters and hot baryons at low redshift. • Absence of large scale peculiar motions: direct confirmation of Copernican principle CosmoRenata meeting, Valencia, June 3rd 2013

  40. The scientific results that we present today are a product of the Planck Collaboration, including individuals from more than 100 scientific institutes in Europe, the USA and Canada Planck is a project of the European Space Agency, with instruments provided by two scientific Consortia funded by ESA member states (in particular the lead countries: France and Italy) with contributions from NASA (USA), and telescope reflectors provided in a collaboration between ESA and a scientific Consortium led and funded by Denmark. CosmoRenata meeting, Valencia, June 3rd 2013

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