Cosmo Renata meeting Valencia June 3 rd 2013

Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

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 Cosmo. Renata meeting, Valencia, June 3 rd 2013

One slide on CMB angular anisotropies … From W. Hu (1998) Gravitational potential well size Cosmo. Renata meeting, Valencia, June 3 rd 2013 # of cold/hot spots in the CMB 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 Ya. B. Zel’dovich R. A. Sunyaev and polarization Materia Radiación 1/ Spot angular size

THE OVERALL PICTURE: Cosmo. Renata meeting, Valencia, June 3 rd 2013

PLANCK VERSUS WMAP ü 10 different channels at 30, 44, 70, 100, 143, 217, 353, 545 and 857 GHz ü Maximum angular resolution of ~0. 075 degrees ü Max. sensitivity of ~0. 25 mu. K per square degree (143 GHz) ID E !! ü 5 different channels at 22, 33, 44, 63, 94 GHz ü Maximum angular resolution of ~0. 23 degrees ü Max. sensitivity of ~5 mu. K per square degree (94 GHz) SL PLANCK, with many more frequency channels and better angular resolution, should: O LD 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 t. SZ source catalog Etc. . . All this should translate into better precision in the cosmological parameters. . . Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

PLANCK 9 BANDS “Cosmological channels” Galactic and extragalactic (Cosmic Infrared emission ) dust emission Cosmo. Renata meeting, Valencia, June 3 rd 2013

Planck 4 algorithms for clean map production Cosmo. Renata meeting, Valencia, June 3 rd 2013

MAP COMPARISON(S) Cosmo. Renata meeting, Valencia, June 3 rd 2013

MAP COMPARISON(S) Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

The angular power spectrum Planck Cosmo. Renata meeting, Valencia, June 3 rd 2013

How Planck got there … • Two different elle regimes: l < 50 and l in [50, 1500] • l<50: Gibbs sampling on all Planck channels • l>50: Two different likelihood estimators: Cam. Spec & Plik, using cosmological channels only [100, 143 and 217 GHz] o Cam. Spec is more accurate and CPU demanding. o Plik does not account for C_l correlation so accurately, but still very useful for running consistency tests • Systematic test at two levels: o 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 o Inter-pair level (involving detectors of different frequencies) – probing foreground related issues Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

Cam. Spec channel pairs … Cosmo. Renata meeting, Valencia, June 3 rd 2013

Camspec VS Plick Cosmo. Renata meeting, Valencia, June 3 rd 2013

Camspec VS Plick (II) Cosmo. Renata meeting, Valencia, June 3 rd 2013

Camspec VS Plick (III) Cosmo. Renata meeting, Valencia, June 3 rd 2013

More consistency tests: 4 clean maps Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

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

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

Basic LCDM cosmological parameter set Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

Cosmological parameter set The case of H 0 : some tension with direct estimates of Hubble constant Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

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 thermal Sunyaev Zel’dovich effect Cosmo. Renata meeting, Valencia, June 3 rd 2013

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

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

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 … Cosmo. Renata meeting, Valencia, June 3 rd 2013

CMB Lensing x 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 Cosmo. Renata meeting, Valencia, June 3 rd 2013

CMB Lensing x galaxy surveys CMB T lensing is correlated to LSS surveys sources at z in [2, 5] Cosmo. Renata meeting, Valencia, June 3 rd 2013

Planck identifies clusters via the t. SZ effect … 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 fewer cold 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 (t. SZ) The symbol y is known as the Comptonization parameter Cosmo. Renata meeting, Valencia, June 3 rd 2013

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 Cosmo. Renata meeting, Valencia, June 3 rd 2013

And in combination with other data … Cosmo. Renata meeting, Valencia, June 3 rd 2013

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 … ? ? ? Cosmo. Renata meeting, Valencia, June 3 rd 2013

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 H 0 test, it alleviates tension between local Hubble estimates and estimates from the CMB Cosmo. Renata meeting, Valencia, June 3 rd 2013

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 Cosmo. Renata meeting, Valencia, June 3 rd 2013

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. Cosmo. Renata meeting, Valencia, June 3 rd 2013