1. Cosmological goals vs measured performances Jean-Loup Puget
The scientific program of Planck
Cosmological goals vs measured performances Jean-Loup Puget
on the behalf of the Planck collaboration
J.L. Puget
Institut d'Astrophysique Spatiale Orsay
on the behalf of the Planck Collaboration
Princeton 21 Feb 2011
J. L. Puget

2. Outline The early Planck papers (arXiv jan 2011):
Overview of in flight Planck performances and data processing
Early Release Compact Source Catalogue
Foreground science
Future foreground science
Cosmological goals vs measured performances
Princeton 21 Feb 2011
J. L. Puget

3. 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.
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.
Princeton 21 Feb 2011
J. L. Puget

4. 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 ( 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.
Princeton 21 Feb 2011
J. L. Puget

5. Noise spectrum of the 10 MW resistor in the focal plane
10 µK/Hz1/2
1µK/Hz1/2
10-4Hz
100 Hz
10-4 Hz
10 Hz
Princeton 21 Feb 2011
J. L. Puget

6. cryogenic chain: the cool down
93 mK July 3rd
2009
Princeton 21 Feb 2011
J. L. Puget

7. Princeton 21 Feb 2011
J. L. Puget

8. Princeton 21 Feb 2011
J. L. Puget

9. Princeton 21 Feb 2011
J. L. Puget

10. 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
PID bolometer plate
average is 5 nW
dilution PID is 25 nW
it is affected by the CR flux and by the small variations of the Helium isotopes flow
small solar flare
10-7 Hz
10-4 Hz
Princeton 21 Feb 2011
J. L. Puget

11. activité solaire 1976 2010 1700 1800 1900 2000 Princeton 21 Feb 2011
J. L. Puget

12. Standard Radiation Monitor
Removing the low energy CR
variations using SREM data
and dilution variations (long term drift
and effect of service module
temperature variations)
Princeton 21 Feb 2011
J. L. Puget

13. Princeton 21 Feb 2011
J. L. Puget

14. following the time ordered data (TOI) processing
Princeton 21 Feb 2011
J. L. Puget

15. Princeton 21 Feb 2011
J. L. Puget

16. Princeton 21 Feb 2011
J. L. Puget

17. Princeton 21 Feb 2011
J. L. Puget

18. 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

19. Sources ERCSC cold ISM concentrations SZ sources: Infrared galaxies
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

20. Contents of ERCSC All sky |b|>30 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
R. Chary: Paris, Jan 2011

21. 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
R. Chary: Paris, Jan 2011

22. ERCSC Sensitivity Planck Galactic Plane |b|<10 deg
Planck Extragalactic
|b|>30 deg
References
C. Beichman et al. 1988
B. Gold et al. 2010
P. Gregory et al. 1996
T. Murphy et al. 2010
E. Wright et al. 2009
R. Chary: Paris, Jan 2011

23. Princeton 21 Feb 2011
J. L. Puget

24. catalogue of 189 clusters detected in SZ
IAP 10 Décmbre 2010
J. L. Puget

25. 3 amas de galaxies en fusion
IAP 10 Décmbre 2010
J. L. Puget

26. electromagnetic content of the universe today
CMB
COpt B
CIB
X-ray B
Gamma B
Radio B
CNES 17 Fevrier 2011
J. L. Puget
H. Dole

27. Power spectrum of the Cosmic Infrared Background
CMB 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. Puget
G. Lagache

28. 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

29. spinning dust in Perseus and rho Oph
SED are different
Princeton 21 Feb 2011
J. L. Puget

30. 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

31. improvements on cosmological parameters over WMAP (blue book)
Princeton 21 Feb 2011
J. L. Puget

32. Planck in combination with other data sets
Princeton 21 Feb 2011
J. L. Puget

33. 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 mK
This happens
at the time of recombination
at « low redshifts » after reionization
Princeton 21 Feb 2011
J. L. Puget

34. Polarization from lensing
Princeton 21 Feb 2011
J. L. Puget

35. Princeton 21 Feb 2011
J. L. Puget

36. 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 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

37. Planck can detect tensor to scalor ratio down to 0
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

38. Princeton 21 Feb 2011
J. L. Puget
J. Tauber: Bogotá, 6 Aug.2009 38