Validation of Planck CMB Power Spectrum & likelihood code

Report
CosmoRenata meeting, Valencia, June 3rd 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
CosmoRenata meeting, Valencia, June 3rd 2013
One slide on CMB angular anisotropies …
From W.Hu (1998)
Gravitational potential well size
CosmoRenata meeting, Valencia, June 3rd 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:
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)
Q band (41 GHz)
Ka band (30 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 7th 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
Contribution from the Cosmic
Infrared Background (CIB)
Anisotropic, galactic signal!
CosmoRenata meeting, Valencia, June 3rd 2013
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)
(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 angular power spectrum
The case of
polarization:
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
Cosmological parameter set
The case of H0 :
some tension with
direct estimates of
Hubble constant
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
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 …
CosmoRenata meeting, Valencia, June 3rd 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
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 SunyaevZel'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 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
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
CITA–ICAT
UNIVERSITÀ DEGLI STUDI
DI MILANO
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CosmoRenata meeting, Valencia, June 3rd 2013
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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