The PLANCK mission

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The PLANCK mission

• on behalf of the
• PLANCK collaboration
• Cécile Renault
• Laboratoire de Physique Subatomique et de
  Cosmologie
• Grenoble - France

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from CMB to cosmology

• COBE T3K large scale anisotropies ? hot BB
• Balloons ground-based experiments
  intermediate scale fluctuations ? inflation
• WMAP large to med. scale T large scale TE
  anisotropies ? concordance model
• Planck will measure large to small scale T E
  anisotropies constrain B-mode fluctuations
• ?
• Precision cosmology,
• new physics ?

Planck 1 year
5 x 5 deg. Field T anisotropies
WMAP 2 years
WMAP 8 years
94 GHz - 15 FWHM
217 GHz - 5 FWHM
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T Power spectra
From pure CMB maps
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E Power spectra
From pure CMB maps
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B-mode sensitivity
From pure CMB maps
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CMB as a powerful tool

• CMB picture of the Universe 380,000 years
  after BB
• temperature predicted by the BB model
• properties strongly linked to inflation
• perturbation generation mechanism
• scale invariance
• ?? 1 predicted

• Enough information to check most of the
  hypotheses
• all sky ? isotropy checked
• known linear physics predicts the distribution ?
  gaussianity checked
• large leverage redshift distribution when
  combined with other observables (clusters,
  supernovae ) to check structure evolution

• Link between cosmology high energy physics
• sound speed at recombination ? Universe content
• neutrinos mass
• footprint of the energy scale of inflation

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Need for accuracy
Blue Book simulations
Comparing concordance ?CDM model with ns 0.95
and no run (solid line) and same ns (at fiducial
wave number k0 0.5 Mpc-1) and run dns/dln k
-0.03
TOP model with no running index simulated
observations with running index
? deviations from a pure scale invariant power
spectrum would provide a firm probe of the
dynamics of an inflationary period
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Cosmological parameters
main parameters better than Precision
predictions measurements ? tests of new
physics become possible
Blue book simulations
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Instrumental challenges Planck solutions

• Tiny signal ? equivalent to the thermal
  emission from a rabbit living on the Moon, as
  seen from Earth, with a human being close to the
  detector
• T ? E ? B signals decreased by orders of
  magnitude
• Significant additive signals from foregrounds

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Bonus a wealth of unique data !

• Measurement of the Sunyaev-Zeldovich effect in gt
  104 galaxy clusters
• gravitational lensing effect
• Radio galaxies, BL Lac objects, quasars
• Low and high redshift dusty galaxies
• Bulk velocities on scales gt 300 Mpc
• Far-infrared background fluctuations
• Evolution of clusters up to z gt 1
• Dust gas distribution in the Milky Way
• Dust properties, cloud cirrus morphology
• Star forming regions, cold molecular clouds
• Galactic magnetic field from synchrotron and
  dust emission
• Study of planets
• Measurements of hundreds of asteroids, comets
• zodiacal light

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The Planck mission

• 1m50 ø telescope
• up to 5 resolution
• Designed for large focal plane and minimal
  intrinsic polarization
• 2 instruments
• Low Frequency Instrument
• 30 to 70 GHz _at_ 20 K
• High Frequency Instrument
• 100 to 857 GHz _at_ 0.1 K

Sensitivity of 2 10-6 ?T/ T
ESA mission first European satellite dedicated
to CMB study HFI PI J.-L. Puget (France) LFI
PI N. Mandolesi (Italy)
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Low Frequency Instrument
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High Frequency Instrument
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The focal plane
The HFI plate (100 to 857 GHz) is surrounded by
LFI horns (30 to 70 GHz)
20 K
0.1 K
In 10-6
In 10-6
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The scanning strategy
From the L2 Lagrange point 30 to 50 times the
same circle, then shift of a third of the
smallest beam ? full sky survey in 7 months
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New but experienced technology
LFI ? WMAP HFI ? Archeops ?
balloon-borne experiment - 12 hour
flight Bolometers _at_ 0.1 K - 143 to 545
GHz polarized channel _at_ 353 GHz
February 7th 2002 flight all references on
www.archeops.org
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Data processing releases

• Computational challenge
• up to 1010 points in the time stream
• 5 107 pixels per map
• Hybrid approaches allow to obtain in a reasonable
  time the most accurate results reducing the
  conceptual simplifications to a minimum.
• Removing systematic effects
• Separating the different components
• ?
• Calibrated timelines
• Maps per frequency
• Maps per component
• Compact source catalogue

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Planck is on the way

• Final assembly _at_Alcatel alenia space
• Spring 2008 last tests at CSL Liege
• Required levels confirmed by calibration
  campaigns

Then launch on Ariane 5 wih Herschel, scheduled
for October 31st 2008
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The cryogenic system
0.1 K plate (HFI)
Main mirror 50 K
1.6 K intermediate stage
Instruments 18 0.1 K
shields 50-60 K (passive cooling)
Service module 300 K
He3
He4
He4
He4
LFI _at_ 18 K - HFI _at_ 0.1 K
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The telescope

• off-axis aplanic design
• 2 elliptical reflectors
• 1.5 m projected ?
• optimized for a large focal plane minimal
  intrinsic polarization
• Operational T 50 K

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Launch orbit
Common launch with Herschel from Kourou by Ariane
V Scheduled for summer 2008
Herschel
Planck