CosmoRenata meeting, Valencia, June 3rd 2013

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
 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

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
Radiación
Materia
From W.Hu (1998)
Gravitational potential well size
CosmoRenata meeting, Valencia, June 3rd 2013
1/ Spot angular size

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

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)
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

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
“Cosmological channels”
Galactic and extragalactic
( Cosmic
Infrared emission
) dust emission
CosmoRenata meeting, Valencia, June 3rd 2013

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

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

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

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

The angular power spectrum
Planck
CosmoRenata meeting, Valencia, June 3rd 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: 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
CosmoRenata meeting, Valencia, June 3rd 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, tSZ & kSZ
Anisotropic, galactic signal!
CosmoRenata meeting, Valencia, June 3rd 2013
Contribution from the Cosmic
Infrared Background (CIB)

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

CosmoRenata meeting, Valencia, June 3rd 2013
Camspec VS Plick

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)
(slight power defect at l ~20, see Vielva’s talk!)
CosmoRenata meeting, Valencia, June 3rd 2013

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

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

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

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

LCDM PARAMETER COMPARISON
From http://lambda.gsfc.nasa.gov
CosmoRenata meeting, Valencia, June 3rd 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 the thermal Sunyaev Zel’dovich effect
CosmoRenata meeting, Valencia, June 3rd 2013

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

CosmoRenata meeting, Valencia, June 3rd 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 …

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 CIB from HFI
CMB T and lensing is correlated to CIB sources at z \in [2,5]
CosmoRenata meeting, Valencia, June 3rd 2013

CMB Lensing x galaxy surveys
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.
Thermal Sunyaev-
Zel'dovich effect
(tSZ)
The symbol y is known as the
Comptonization parameter
CosmoRenata meeting, Valencia, June 3rd 2013

Catalogue of >1,227 SZ Galaxy Clusters
New thermal SunyaevZel’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 N eff
~ 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
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
CosmoRenata meeting, Valencia, June 3rd 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
U NIVERSITÀ DEGLI S
DI
M
ILANO
CIT
A – ICAT
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