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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 - PowerPoint PPT Presentation
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CosmoRenata meeting, Valencia, June 3rd 2013
Planck's Main Results
Carlos Hernández-Monteagudo
Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Teruel, SpainOn 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
CosmoRenata meeting, Valencia, June 3rd 2013
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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
From W.Hu (1998)
RadiaciónMateria
Gravitational potential well size
Ya.B.Zel’dovich R.A.Sunyaev
One slide on CMB angular anisotropies …
CosmoRenata meeting, Valencia, June 3rd 2013
THE OVERALL PICTURE:
CosmoRenata meeting, Valencia, June 3rd 2013
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...
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)
CosmoRenata meeting, Valencia, June 3rd 2013
OLD SLIDE !!
CosmoRenata meeting, Valencia, June 3rd 2013
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
PLANCK 9 BANDS
Galactic and extra-galactic (Cosmic Infrared emission) dust emission
“Cosmological channels”
CosmoRenata meeting, Valencia, June 3rd 2013
Planck 4 algorithms for clean map production
MAP COMPARISON(S)
CosmoRenata meeting, Valencia, June 3rd 2013
MAP COMPARISON(S)
CosmoRenata meeting, Valencia, June 3rd 2013
The angular power spectrum
CosmoRenata meeting, Valencia, June 3rd 2013
WMAP 7th year
The angular power spectrum
CosmoRenata meeting, Valencia, June 3rd 2013
Planck
How Planck got there …
CosmoRenata meeting, Valencia, June 3rd 2013
• 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: CamSpec & Plik, using cosmological channels only [100, 143 and 217 GHz]o CamSpec 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
Getting rid of galactic dust …
CosmoRenata meeting, Valencia, June 3rd 2013
Use 857 GHz as template for galactic dust + CIB template (derived from data) + theoretically motivated templates for Poisson, clustered, tSZ & kSZ
Anisotropic, galactic signal!
Contribution from the Cosmic Infrared Background (CIB)
CamSpec channel pairs …
CosmoRenata meeting, Valencia, June 3rd 2013
Camspec VS Plick
CosmoRenata meeting, Valencia, June 3rd 2013
Camspec VS Plick (II)
CosmoRenata meeting, Valencia, June 3rd 2013
Camspec VS Plick (III)
CosmoRenata meeting, Valencia, June 3rd 2013
More consistency tests: 4 clean maps
CosmoRenata meeting, Valencia, June 3rd 2013
The low elle part … (Commander)
CosmoRenata meeting, Valencia, June 3rd 2013
(slight power defect at l ~20, see Vielva’s talk!)
The Final angular power spectrum
CosmoRenata meeting, Valencia, June 3rd 2013
Planck vs other exps.
The angular power spectrum
CosmoRenata meeting, Valencia, June 3rd 2013
The case of polarization:
Basic LCDM cosmological parameter set
CosmoRenata meeting, Valencia, June 3rd 2013
Strong limits on NG
CosmoRenata meeting, Valencia, June 3rd 2013
Very Gaussian universe, no hint for non Gaussianity after correcting for the coupling of the lensing with the ISW …
A lot of inflationary models ruled out …
See Vielva’s talk!
Cosmological parameter set
CosmoRenata meeting, Valencia, June 3rd 2013
The case of H0 : some tension with direct estimates of Hubble constant
LCDM PARAMETER COMPARISON
CosmoRenata meeting, Valencia, June 3rd 2013
From http://lambda.gsfc.nasa.gov
There is a lot of secondary Science …
CosmoRenata meeting, Valencia, June 3rd 2013
• 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 Sunyaev Zel’dovich effect
Secondary anisotropies == Anisotropies introduced along the CMB photon’s way to us by gravitational potential wells, scattering with electrons, etc
CMB Lensing
CosmoRenata meeting, Valencia, June 3rd 2013
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:
CMB Lensing (II)
CosmoRenata meeting, Valencia, June 3rd 2013
(Left) Simulated 2D potential field reconstruction
(Below) Real 2D potential field reconstruction
CMB Lensing (III)
CosmoRenata meeting, Valencia, June 3rd 2013
(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 …
CMB Lensing x CIB from HFI
CosmoRenata meeting, Valencia, June 3rd 2013
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
CMB Lensing x galaxy surveys
CosmoRenata meeting, Valencia, June 3rd 2013
CMB T lensing is correlated to LSS surveys sources at z \in [2,5]
CosmoRenata meeting, Valencia, June 3rd 2013
Planck identifies clusters via the tSZ 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.
The symbol y is known as the Comptonization parameter
Thermal Sunyaev-Zel'dovich effect (tSZ)
Catalogue of >1,227 SZ Galaxy Clusters
CosmoRenata meeting, Valencia, June 3rd 2013
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
And in combination with other data …
CosmoRenata meeting, Valencia, June 3rd 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 …
???
CosmoRenata meeting, Valencia, June 3rd 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 H0 test, it alleviates tension between local Hubble estimates and estimates from the CMB
CosmoRenata meeting, Valencia, June 3rd 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
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