The scientific program
Cosmological
goals
of Planck
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
Outline
1. 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
Princeton 21 Feb 2011
J. L. Puget
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
cosmology.
PrincetonCMB
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.
Princeton 21 Feb 2011
J. L. Puget
Noise spectrum of the 10 MW resistor in the focal plane
10 µK/Hz1/2
1µK/Hz1/2
10-4Hz
10-4 Hz
Princeton 21 Feb 2011
10 Hz
J. L. Puget
100 Hz
cryogenic chain: the cool down
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
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
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
Princeton 21 Feb 2011
J. L. Puget
10-4 Hz
• activité solaire
1976
Princeton 21 Feb 1800
2011
1700
2010
1900
J. L. 2000
Puget
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
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
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
Contents of ERCSC
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
All sky
|b|>30
705
307
452
143
599
157
1381
332
1764
420
5470
691
6984
1123
•
•
*fluxmap.pdf: Sky distribution with flux information
ERCSC cutouts and PSF cutouts: 4*FWHM CMB subtracted maps.
7223
2535
8988
4513
•
•
•
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
20/24
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
R. sensitivity
Chary: Paris, compared
Jan 2011
• Improved spatial resolution and
to WMAP in the radio
21/24
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
22/24
R. Chary: Paris, Jan 2011
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
CMB
CIB
COpt B
X-ray B
Gamma B
Radio B
CNES 17 Fevrier 2011
J. L. Puget
H. Dole
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
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
Planck in combination with other
data sets
Princeton 21 Feb 2011
J. L. Puget
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
Polarization from lensing
Princeton 21 Feb 2011
J. L. Puget
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
Princeton 21 Feb 2011
J. L. Puget
J. Tauber: Bogotá, 6 Aug.2009