Princeton 21 Feb 2011 J. L. Puget

Cosmological goals vs

measured performances

Jean-Loup Puget

J.L. PugetInstitut d'Astrophysique Spatiale

Orsay

on the behalf of the Planck Collaboration

The scientific program of Planck

on the behalf of the Planck collaboration

Princeton 21 Feb 2011 J. L. Puget

Outline1. The early Planck papers (arXiv jan 2011):

1. Overview of in flight Planck performances and data processing

2. Early Release Compact Source Catalogue

3. Foreground science

2. Future foreground science

3. Cosmological goals vs measured performances

The Planck Collaboration is composed of - a core: the Pl. Sc. Off., the two instruments Core Teams and the telescope team. They are in charge of producing the scientific products distributed to the scientific community and the first set of papers on CMB cosmology.- it also includes associates from more than 50 scientific institutes in Europe, the USA and Canada who are contributing to the scientific program outside CMB cosmology.

Planck is a project of the European Space Agency -- ESA -- 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.

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

Planck: the 3rd generation space CMB experiment

• Planck has the ambition to gain a factor 2.5 in angular resolution and 10 in instantaneous map sensitivity with respect to WMAP

• Planck will be nearly photon noise limited in the CMB channels (100-200 GHz)

• Temperature power spectrum sensitivity should be limited by the ability to remove foregrounds (thus a very broad frequency coverage: 30 GHz-1 THz)

• HFI detectors are cooled to 100 mK, 6 bands 100 to 857 GHz, read in total power mode with a white noise from 10 mHz to 100 Hz (no 1/f noise from readout electronics in the signal range)

• the temperature stability of the 100 mK stage must be better that 20 nK/rt-Hz in the same band not to affect the sensitivity

• LFI uses coherent detection and HEMTS based amplifiers in 3 bands 30 to 70 GHz, photometric reference loads on the 4K box of the HFI FPU with micro K stability.

Noise spectrum of the 10 M resistor in the focal plane

Princeton 21 Feb 2011 J. L. Puget

10-4 Hz 10 Hz

10 µK/Hz1/2

10-4Hz 100 Hz

1µK/Hz1/2

cryogenic chain: the cool down

Princeton 21 Feb 2011 J. L. Puget

93 mK July 3rd

2009

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

the100mK bolometer plate PID power fluctuations follows closely the opposite of the

SREM particle counts fluctuations • total power from CR on bolometer plate is 12 nW

Princeton 21 Feb 2011 J. L. Puget

PID bolometer plateaverage is 5 nW

dilution PID is 25 nWit is affected by the CR flux and by the small variations of the Helium isotopes flow

small solar flare

10-4 Hz10-7 Hz

• activité solaire

1976 2010

1700 1900 20001800Princeton 21 Feb 2011 J. L. Puget

Standard Radiation Monitor

Princeton 21 Feb 2011 J. L. Puget

Removing the low energy CR variations using SREM data and dilution variations (long term driftand effect of service module temperature variations)

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

following the time ordered data (TOI) processing

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

The Planck scientific program: foregrounds• sources

– rising spectra radio sources

– infrared galaxies (SED of galaxies, high z sources, star formation history)

– SZ sources

• interstellar medium– tracing dust foreground (new dust opacity all sky map, rotation of

PAHs and VSG)

– full sensus of cold spots in the ISM

– dust properties in the mm submm spectral range including polarization

– structure of the galactic magnetic field (particularly the statistical properties of the turbulent field)

– Princeton 21 Feb 2011 J. L. Puget

Sources• ERCSC• cold ISM concentrations • SZ sources:

– 5 arc min is too a low resolutionto be competitive with some ground based experiments (SPT,ACT, interferometers)

– all sky is very good for rare sources (very massive clusters, high z), stacking of sources from other catalogues

– power spectrum of unresolved sources background at intermediate l from Planck will complement SPT, ACT

• Infrared galaxies– CIB

– high z rare objects (proto clusters) Princeton 21 Feb 2011 J. L. Puget

Catalogs from Intensity Maps• ERCSC_f030.fits• ERCSC_f044.fits • ERCSC_f070.fits• ERCSC_f100.fits• ERCSC_f143.fits• ERCSC_f217.fits • ERCSC_f353.fits • ERCSC_f545.fits• ERCSC_f857.fits with bandfilled info at 217, 353 and 545 GHz

• *fluxmap.pdf: Sky distribution with flux information• ERCSC cutouts and PSF cutouts: 4*FWHM CMB subtracted maps.

• ECC.fits (915 entries; 35 at |b|>30)• Planck_ECC.pdf: ECC cutouts on 353, 545 and 857 residual maps; 0.33 deg on

a side• ECC_skymap.pdf: Sky distribution of ECC candidates

• ESZ.fits (189 sources; 134 at |b|>30)• ESZ_skymap.pdf: Sky distribution of ESZ candidates

• Explanatory Supplement

All sky |b|>30

705 307

452 143

599 157

1381 332

1764 420

5470 691

6984 1123

7223 2535

8988 4513

Contents of ERCSC

R. Chary: Paris, Jan 201120/24

R. Chary: Paris, Jan 2011

Features of Planck

• Unique phase space – the first simultaneous radio through submillimeter all sky survey

- Fills in the gap in phase space between WMAP and Akari/IRAS- Probes both the dusty infrared luminous sources and the synchrotron sources

• Spatial resolution well matched to IRAS at 3 longer wavelengths• Improved spatial resolution and sensitivity compared to WMAP in the radio

21/24

ERCSC Sensitivity

R. Chary: Paris, Jan 2011

Planck Galactic Plane |b|<10 deg

Planck Extragalactic|b|>30 deg

ReferencesC. Beichman et al. 1988B. Gold et al. 2010P. Gregory et al. 1996T. Murphy et al. 2010E. Wright et al. 2009

22/24

Princeton 21 Feb 2011 J. L. Puget

catalogue of 189 clusters detected in SZ

IAP 10 Décmbre 2010 J. L. Puget

3 amas de galaxies en fusion

IAP 10 Décmbre 2010 J. L. Puget

electromagnetic content of the universe today

H. Dole

CMB

CIB COpt B

X-ray B

Gamma B

Radio B

CNES 17 Fevrier 2011 J. L. Puget

Power spectrum of the Cosmic Infrared BackgroundCMB is the main contaminant CMB/CIB=1000 at l=200

• the CIB power spectrum illustrates the power of the Planck data for component separation and CMB work

• at 217 GHz the measured CIB power spectrum l Cl is 0.25 µK2 with a S/N of 5 on 100 sq deg

CNES 17 Fevrier 2011 J. L. PugetG. Lagache

interstellar medium • cold gas and B field substructure of interstellar filaments• turbulent magnetic field• rotation of PAHs and very small grains

IAP 10 Décmbre 2010 J. L. Puget

spinning dust in Perseus and rho Oph

• SED are different

Princeton 21 Feb 2011 J. L. Puget

Planck scientific program: CMB • refining cosmological parameters by a factor 10 to 30 to test for

tensions in the cosmological parameters issued from WMAP and other cosmological probes (reionization history)

• neutrino mass (upper limits can be lowered by a factor of 4 to 5)

• search for B modes from inflation gravity waves; test compatibility with ns predicted by simple inflation models

• non gaussianity: – test of inflation models,

– of non inflationary models (non trivial topology on large scales)

– lensing

Princeton 21 Feb 2011 J. L. Puget

improvements on cosmological parameters

over WMAP (blue book)

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

Planck in combination with other data sets

Indirect observation of primordial gravity waves

• They imprint polarization on the CMB from Compton interaction with ionized gaz affected by the gravity waves

• r = 0.1 leads to rms of Bmodes 0.06 K

• This happens – at the time of recombination– at « low redshifts » after reionization

Princeton 21 Feb 2011 J. L. Puget

Princeton 21 Feb 2011 J. L. Puget

Polarization from lensing

Princeton 21 Feb 2011 J. L. Puget

Primordial B-mode detection• Efstathiou, Gratton 2009• using Planck Sky Model (full sky simulation but

rather simple model of foregrounds)• nominal sensitivity and extended mission (4 sky

surveys vs 2)• takes simple inflation model predictions

– r = 0, 0.05, 0.1 (energy scale 1.4 1016 GeV for r = 0.05 with ns=0.96)

– can we detect the predicted B modes?

• after a simple component separation assuming no systematic effects

Princeton 21 Feb 2011 J. L. Puget

• Planck can detect tensor to scalor ratio down to 0.05 (present best direct upper limit is 0.3 one sigma, Bicep Chiang et al 2009)

Princeton 21 Feb 2011 J. L. Puget

J. Tauber: Bogotá, 6 Aug.2009

Princeton 21 Feb 2011 J. L. Puget