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The Planck Satellite Hannu Kurki-Suonio University of Helsinki

The Planck Satellite Hannu Kurki-Suonio University of Helsinki. Finnish-Japanese Workshop on Particle Cosmology, Helsinki 8-9.3.2007. Structure in the Cosmic Microwave Background. COBE, launched 1989. Polar orbit, 900 km altitude. WMAP, launched 2001.

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The Planck Satellite Hannu Kurki-Suonio University of Helsinki

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  1. The Planck SatelliteHannu Kurki-SuonioUniversity of Helsinki Finnish-Japanese Workshop on Particle Cosmology, Helsinki 8-9.3.2007

  2. Structure in the Cosmic Microwave Background COBE, launched 1989 Polar orbit, 900 km altitude WMAP, launched 2001 In orbit around L2 point of Sun-Earth system 1.5 million km from Earth in the anti-Sun direction

  3. WMAP 3-year angular power spectrum + smaller scale suborbital experiments 2006 Angular power spectrum 1996 (Tegmark, ApJ 464, L35) 2006 Standard cosmology 2006: Big bang + cold dark matter + dark energy + inflation (primordial density perturbations probably generated by quantum fluctuations during inflation)

  4. Planck Herschel • European Space Agency (ESA) satellite, to be launched from Kourou, French Guyana, with Ariane 5 rocket • NASA participates • Collaboration of about 10 European countries, • France, Italy, UK, Spain, Germany, Finland, Switzerland, Norway, ... • USA, and Canada • High Frequency Instrument (HFI) • Low Frequency Instrument (LFI) • Finnish science participation: • Univ. Helsinki (cosmology, astronomy) • TKK (astronomy) • Univ. Turku (astronomy) Planck

  5. Planck satellite (ESA) • Launch in 2008 • Orbit around L2 • Surpasses WMAP in • resolution 5 vs 14 arcmin • sensitivity: CMB polarization • frequency coverage: foreground separation

  6. Planck measures the microwave sky at 9 frequencies Detectors built in Finland MilliLab (VTT & TKK) and Ylinen Electronics Low Frequency Instrument (LFI): 30, 44, 70 GHz High Frequency Instrument (HFI): 100, 143, 217, 353, 545, 857 GHz LFI HFI HFI

  7. Sunyaev-Zeldovich effect

  8. Polarization • 7 channels (all except 545, 857GHz) measure polarization • Probes different physics than temperature anisotropies • picks up signal only from photon scattering • no integrated Sachs-Wolfe effect • sensitive to reionization (low multipoles) • Breaks degeneracies • Signal weaker (the high sensitivity of Planck needed) • E and B modes • B mode comes from tensor perturbations (Planck may detect if r ~ 0.1) and lensing of E mode (high multipoles)

  9. TE spectrum projected Planck data projected Boomerang and 4-year WMAP data actual Boomerang data actual WMAP 3-year data

  10. EE spectrum projected Boomerang and 4-year WMAP data projected Planck data actual Boomerang data actual WMAP 3-year data

  11. BB spectrum lensing of E mode reionization bump tensor perturbations existing WMAP 3-year data projected Planck data (assumes r = 0.1)

  12. Planck at Alcatel (Cannes, France) - almost complete - telescope mirrors not yet attached

  13. Timetable (estimated) • August 2008: Launch • January 2009 – March 2010: Scientific data taking • Extension possible • March 2010 – March 2012: proprietary period • data analyzed, Planck publications prepared • March 2012: Planck data in the public domain

  14. Data Analysis Pipeline Raw data Cleaning, calibration Time-ordered data Map-making 9 frequency maps (3 LFI, 6 HFI) Component separation Component maps: CMB, foregrounds Power spectrum estimation Angular power spectra Parameter estimation Cosmological parameters W, wb, wcdm, WL, H0, A, ns, r, t

  15. Science from Planck • Cosmological parameters determined to high accuracy • Current (WMAP + other) data consistent with a “concordance” model of cosmology with 6 parameters • Assuming this concordance model: • wb, wcdm, WL, A known already to good accuracy • ns, tnot known well before Planck • Deviations from the concordance model • additional parameters (pre-Planck data mostly not enough) • Inflation parameters: ns, r, dns /d ln k • select among inflation models • Nature of primordial perturbations (adiabaticity) • how they were generated • Non-gaussianity, check WMAP large-scale anomalies

  16. Current (WMAP) constraints on inflation models Spergel et al (2006)

  17. astro-ph/0611917 astro-ph/0702223 Dc2 = -9.6 with 4 extra parameters Dc2 = -3.9 with 1 extra parameter

  18. Conclusion: Exciting times ahead!

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