cosmological results from planck

Cosmological Resultsfrom Planck

Marian DouspisIAS-Orsay

1

CITA – ICAT

UNIVERSITÀ DEGLI STUDIDI MILANO

ABabcdfghiejkl

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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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M. Douspis, 01/07/2013, Cosmology Results from Planck 3

• Planck

• Maps

• CMB Likelihoood

• CMB Results on LCDM

• CMB results on extentions

• LSS results

• Next....

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M. Douspis, 01/07/2013, Cosmology Results from Planck

Planck

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Launch: May 14 2009

• 2 Instruments HFI+LFI• Observation in 9 frequency bands• 22 radiometers (LFI) and 56 sensitive / fast bolometers (HFI)

• 5 stages cryogenic cooling chain

• Aug. 2009: survey started• Nov. 2010: nominal mission (2 surveys) achieved

• Mid-Jan. 2012: extended cryogenic mission (5 surveys) achieved

• Summer 2013: warm mission achieved

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Why Planck ?

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At decision time (~1992)

At launch

At my PhD (~2000)

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Why Planck ?

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Probing large and small scales with same instrument to avoid calibration problems

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Why Planck ?

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WMAP SPT

Probing low and high frequencies to have a better handle on contaminating foregrounds

30 44 77 100 143 217 353 545 857

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Planck-HFI: technological success

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1.6 K

Cryostat He3/He4

Extremely complex but extremely stable cryogenic chain

100 mK

4 K

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Planck: data analysis success

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143 GHz

545 GHz

blind bolometer

Galaxycosmics

Dipole

33GHz 44GHz 70GHz

100GHz 143GHz 217GHz

353GHz 545GHz 857GHz

800 GB from L21010 sample per bolometer5.107 pixels per map

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Planck: Scientific success

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Early Results• Release of Point sources and SZ catalogues• based on 11 month of data• 27 papers

Results • Release of maps, catalogues, ...• based on 14 month of data• 28 papers

Intermediate Results • based on 11 month of data• 13 papers

2011 2013

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Some press coverage

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March 21st or 22nd, 2013

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2011+2013 Release

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• Maps per frequency

• CMB maps

• component maps

• Lensing map

• Dust opacity map

• point sources catalogues

• SZ catalogue

• Likelihood ...

PLA: Planck Legacy Archive:http://pla.esac.esa.int/pla/aio/planckProducts.html

LAMBDA:http://lambda.gsfc.nasa.gov

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• Planck

• Maps

• CMB Likelihoood



• LSS results

• Next....

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2013 Results

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Low frequency CO Dust

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Planck CMB map

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From M. Tristram

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From M. Tristram

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From M. Tristram

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Angular power spectrum

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CMB from space

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Cosmology

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• Amplitude of the fluctuations mostly from the plateau

• Sound horizon: first peak location

• Total matter: changes the contrast between the peaks

• Baryon density: changes the ratio between peak heights (inertia)

• Reionisation optical depth: damps small scales. Constrained from large scale polarisation but also marginally from lensing

• H0: derived from above parameters

• Curvature: large scales (ISW) small scales (lensing) ‏

• Neutrino masses: small scales (lensing)

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• Planck

• Maps

• CMB Likelihoood



• LSS results

• Next....

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Likelihood large scales• pixel based likelihood for l=[2,49]

• CMB map @ low resolution

• 4 algorithms: very similar results

• Error: dominated by cosmic variance

• Anomaly: points lower than best model, no effect on cosmology

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Likelihood small scales• Cl likelihood for l=[50,2500]

• power spectra of maps @ 100, 143, 217 GHz

• No foreground cleaning in maps, but optimized masks and l-regions

• Modelling of CMB+contaminants

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Likelihood

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Cmodel

`

= CCMB

`

+ Cdust

`

+ Ccib+sz

`

+ Cpoisson

`

+ Cksz

`

Cmodel

`

? ⌘? Cdata

`

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• Planck

• Maps

• CMB Likelihoood



• LSS results

• Next....

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ΛCDM• 6 parameters

• 2 primordial spectrum

• 1 expansion rate

• 2 paramaters for densities

• reionization

• Hypothesis (relaxed for extension)

• Flat Universe• No running• No tensor

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• 3 neutrinos species

• Standard neutrinos with low mass

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Results• +WP : WMAP polarisation (TE+EE @ low-l)

‣ breaks As-tau degeneracy

• +HighL : +SPT+ACT for l in [2000,2500]

‣ better foreground handling

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Standard cosmology

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18 fold diminution in constraint volume compared to WMAP9 + SPT33 marginalised nuisance + foreground parameters

%-level cosmologySimple LCDM model works remarkably well

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Heavier and older Universe

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H0.............. 70.0 + 2.2 67.80 ± 0.77Age............. 13.74 + 0.11 13.798 ± 0.037

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(dis)agreement

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Error bars divided by 2

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(dis)agreement

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100 500 1000 2000Multipole moment �

0

500

1000

1500

�2 D�[m

K2 ]

ns = 0.96ns = 1.00

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Inflation

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Starting to exclude some inflation modelsScale invariant perturbation clearly excluded

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Inflation

• Measuring bispectrum: Search for specific shapes in the 3pt correlation function → Local type

• WMAP9 constraints on nonlinearity parameter fNL local = 37 ± 20

• Upper bound limits extensions of singl-field slow role inflation models

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• Planck

• Maps

• CMB Likelihoood



• LSS results

• Next....

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Curvature

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Flat Universe

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Other implications

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• q: sound horizon is determined by the position of the 7 peaks, and now measured at 0.05% precision

• spatially flat Universe

• ns: exact scale invariance of the primordial fluctuations is ruled out, at more than 7s (as predicted by base inflation models)

• Nucleosynthesis ok

• Upper limit on neutrino masses

• 3 neutrinos species favored by Planck

• no evidence for dynamical dark energy• no evidence for running index dns/dlnk

q = 1.04147± 0.00056

ns = 0.9608± 0.0054

Xm⌫ < 0.23eV

Neff = 3.30+0.54�0.51

Yp = �0.267± 0.044

⌦k = �0.0007± 0.0033

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Cosmological model established with exquisit CMB

but

Planck is not only a CMB machine !

Planck probes:

Dark matter distribution → CMB lensing Hot gas content → Sunyaev-Zel'dovich effectStar formation → Cosmic IR Background

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CMB lensing: matter tracer• Gravitational effect of the

LSS @ z=2 affects the observed CMB

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CMB lensing detected at 25σ

significance

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CMB lensing: matter tracer

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• Reconstructed projected mass map

• Correlation with external tracers agrees well

Planck LCDM in agreement with z=2 structures

Quasars – z ~ 1 Galaxy clusters – z ~ 0.2

Galaxies – z~ 0.5 Galaxies – z ~ 0.1

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CIB: galaxy tracer

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• This maps primarily show the Cosmic Infrared Background, emission from warm dust in distant star-forming galaxies at redshifts between 1 and 3

• CIB = HFI - dust - CMB - PointSources

• Sub-degree clustered structures correlate between frequencies Southern cap at 353 GHz

results 2011

201140deg2

2013>1000deg2

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CIBxlensing: dark matter tracer

Stacking the Planck mass maps at the positions of peaks and troughs of Cosmic Infrared Background leads to a strong detection of the mass associated with these distant star forming galaxies. This is mostly Dark Matter.

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1º

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SZ effect: hot baryon tracer

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Electron énergétique

Amas de Galaxies: galaxies + gaz

CMB photon

Photon diffusé plus chaud

R. A. Sunyaev Ya. B. Zeldovich

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SZ effect: hot baryon tracer

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Electron énergétique

Amas de Galaxies: galaxies + gaz

CMB photon

Photon diffusé plus chaud

R. A. Sunyaev Ya. B. Zeldovich

“Hole in the sky”

SZ,Comments on Astrophysics and Space Physics 1972

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Planck: SZ machine

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Planck SZ catalogue

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• PSZ based on [100-857]GHz maps

• 3 detection algorithms

• on ~84% of the sky

• 1227 clusters & candidates

• 683 previously known

• 178 new clusters• 366 candidates

• z in [0-1]

• M in [1~20] 1014 M☉• Mmed ~ 3.5 1014 M☉

• see Planck 2013 XXIX & PLA

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SZ cluster number counts

• Reference mass function: Tinker et al.

• Reference scaling Y-M: based on 71 Planck clusters

• Reference selection function: based on Planck noise maps

• Reference sample: S/N selected sample of 189 PSZ clusters

Internal consistency: use mostly Planck information

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(1-b): bias between hydrostatic equilibrium mass and total mass

0.50 2.0

-120

-600

60120

-75

-60

-45

-30

-15

0

15

30

45

60

75

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Constraints from SZ counts

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SZ+BAOSZ+HST

degeneracy �8(⌦m/0.29)0.32

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M. Douspis, 03/04/2013, Cosmology from Planck SZ cluster counts

Robustness• Reference run (SZ+BAO)

• S/N>8 sample

• MMF1 sample

• MC-based completeness

• Reference run (SZ+BAO)

• Free redshift evolution of scaling

• Watson et al. mass function

• (1-b) in [0.7-1.0]

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95% CL

95% CL

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Coherent view from clusters

• Comparison with some Optical, X-rays, SZ constraints using clusters

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0.

700.

750.

800.

850.

900.

95

m8(1

M/0

.27)

0.3

WL*

X-rays*

MaxBCG*

ACT

SPTPlanck

Planck

SPT

WMAP

Clusters CMBLSS

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Comparison with CMB• Higher values of Ωm,σ8 in

Planck CMB analysis

• 3σ tension

• More general tension between clusters and CMB ?

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SZ+BAOCMB

0.

700.

750.

800.

850.

900.

95

m8(1

M/0

.27)

0.3

WL*

X-rays*

MaxBCG*

ACT

SPTPlanck

Planck

SPT

WMAP

Clusters CMBLSS

100

101

102

0.0 0.2 0.4 0.6 0.8 1.0z

dNdz

Best model from Planck CMBBest model from y-mapBest modelPlanck counts

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SZ counts & CMB• Getting higher σ8 from clusters

• Change scaling

• Change bias

• Account for missing clusters

• Getting lower σ8 from CMB

• Change initial power spectrum

• Change transfert function

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SZ counts & CMB• Higher σ8 in clusters

• (1-b)=0.55

• open question on baryons

• Only few missed clusters

• Lower σ8 in CMB

• running not enought

• massive neutrino

• 2 possible solutions that reconcile SZ & CMB

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SZ+CMB, b = 0.8SZ+CMB, b in [0.7-1]CMB

SZ+CMB+BAO, b [0.7-1]

SZ+CMB, b freeSZ+BAOCMB

0.2

0.4

0.6

0.8

1.0

0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4Y mi

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All sky map of the SZ signal• Adap ted componen t

separation methods based on:• constraints on emission

spectra + localisation in pixel and multipole domains

• 100 to 857GHz channel maps

• Resolved SZ clusters (from PSZ catalogue) account for a significant fraction of the tSZ signal in the reconstructed maps

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Coma O

North South

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Constraints from SZ map• Three component model on

50% of the sky:

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Cmodel

`

= CSZ

`

+ Ccib

`

+ CPS

`

First measure of SZ spectra from large to small scales

Consistency with cluster counts cosmology

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And much more...• Anomalies

• ISW

• proto-clusters

• Galaxy

• ...

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• Planck 2013 results. I. Overview of products and results

• Planck 2013 results. II. Low Frequency Instrument data processing

• Planck 2013 results. III. LFI systematic uncertainties

• Planck 2013 results. IV. LFI beams

• Planck 2013 results. V. LFI calibration

• Planck 2013 results. VI. High Frequency Instrument data processing

• Planck 2013 results. VII. HFI time response and beams

• Planck 2013 results. VIII. HFI calibration and mapmaking

• Planck 2013 results. IX. HFI spectral response

• Planck 2013 results. X. HFI energetic particle effects

• Planck 2013 results. XI. Consistency of the data

• Planck 2013 results. XII. Component separation

• Planck 2013 results. XIII. Galactic CO emission

• Planck 2013 results. XIV. Zodiacal emission

• Planck 2013 results. XV. CMB power spectra and likelihood

• Planck 2013 results. XVI. Cosmological parameters

• Planck 2013 results. XVII. Gravitational lensing by large-scale structure

• Planck 2013 results. XVIII. The gravitational lensing-infrared background correlation

• Planck 2013 results. XIX. The integrated Sachs-Wolfe effect

• Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts

• Planck 2013 results. XXI. All-sky Compton-parameter map and characterization

• Planck 2013 results. XXII. Constraints on inflation

• Planck 2013 results. XXIII. Isotropy and statistics of the CMB

• Planck 2013 results. XXIV. Constraints on primordial non-Gaussianity

• Planck 2013 results. XXV. Searches for cosmic strings and other topological defects

• Planck 2013 results. XXVI. Background geometry and topology of the Universe

• Planck 2013 results. XXVII. Special relativistic effects on the CMB dipole

• • Planck 2013 results. XXVIII. The Planck Catalogue of Compact Sources • Planck 2013 results. XXIX. The Planck catalogue of Sunyaev-Zeldovich sources

• Planck 2013 results. Explanatory supplement

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Conclusions• Planck CMB sets the new

standard LCDM

• No extended LCDM needed

• Agreement with small scales CMB, SN-union, BAO, lensing x-correlations

• Tension with HST/H0, clusters and SZ spectrum

• large scale anomaly ?

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• Planck probes z~1000

• but also

• Dark matter z≾2

• Baryons/gas z≾1

• Baryons/light z~2-3

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Coming next• in 2014 !

• 15 → 30 month

• Polarisation

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Thank you !

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