Planck 's Main Results
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Transcript of Planck 's Main Results
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Planck's Main Results
Carlos Hernández-Monteagudo
Centro de Estudios de Física del Cosmos de Aragón (CEFCA), Teruel, SpainOn behalf of the Planck collaboration
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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
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# of
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1/ Spot angular size
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 …
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THE OVERALL PICTURE:
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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)
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OLD SLIDE !!
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WMAP 5 bands
K band (23 GHz) Ka band (30 GHz)
Q band (41 GHz) V band (61 GHz)
W band (94 GHz)
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PLANCK 9 BANDS
Galactic and extra-galactic (Cosmic Infrared emission) dust emission
“Cosmological channels”
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Planck 4 algorithms for clean map production
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MAP COMPARISON(S)
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MAP COMPARISON(S)
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The angular power spectrum
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WMAP 7th year
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The angular power spectrum
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Planck
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How Planck got there …
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• 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
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Getting rid of galactic dust …
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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)
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CamSpec channel pairs …
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Camspec VS Plick
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Camspec VS Plick (II)
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Camspec VS Plick (III)
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More consistency tests: 4 clean maps
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The low elle part … (Commander)
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(slight power defect at l ~20, see Vielva’s talk!)
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The Final angular power spectrum
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Planck vs other exps.
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The angular power spectrum
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The case of polarization:
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Basic LCDM cosmological parameter set
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Strong limits on NG
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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!
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Cosmological parameter set
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The case of H0 : some tension with direct estimates of Hubble constant
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LCDM PARAMETER COMPARISON
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From http://lambda.gsfc.nasa.gov
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There is a lot of secondary Science …
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• 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
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CMB Lensing
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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:
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CMB Lensing (II)
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(Left) Simulated 2D potential field reconstruction
(Below) Real 2D potential field reconstruction
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CMB Lensing (III)
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(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 …
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CMB Lensing x CIB from HFI
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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
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CMB Lensing x galaxy surveys
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CMB T lensing is correlated to LSS surveys sources at z \in [2,5]
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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)
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Catalogue of >1,227 SZ Galaxy Clusters
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New thermal Sunyaev-Zel’dovich clusters are mostly nearby, massive objects that are un-relaxed and hence with low X-ray emission
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And in combination with other data …
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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 …
???
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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
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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
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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.
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