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Planck Satellite Revisited

Planck Satellite Revisited. Anne Lähteenmäki Metsähovi Radio Observatory Helsinki University of Technology TKK. CMB missions. Planck 2010 5’  30’. 7 . 0.3 . Planck ― ESA. Launch in January 2009 together with Herschel satellite ~4 months to reach L2 Whole sky covered once in

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Planck Satellite Revisited

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  1. Planck Satellite Revisited Anne Lähteenmäki Metsähovi Radio Observatory Helsinki University of Technology TKK

  2. CMB missions Planck 2010 5’  30’ 7 0.3

  3. Planck ― ESA • Launch in January 2009 together with Herschel satellite • ~4 months to reach L2 • Whole sky covered once in 6 months → several cycles

  4. Payload • Two instruments, 9 frequencies + polarization: • Low Frequency Instrument LFI (30 – 77 GHz), 20 K • High Frequency Instrument HFI (100 – 857 GHz), 0.1 K

  5. The supremacy of Planck • more frequencies • higher resolution • higher sensitivity (also polarization)

  6. Planck foregrounds • Identification and elimination of contaminating foreground radio sources • ”Garbage for cosmologists = science for astronomers!” • Planck will produce the most complete radio source catalogs ever at high radio frequencies (30 -857 GHz)

  7. Planck foregrounds • complete samples of all classes of radio sources, possibly also new source types • statistical studies, classification of sources... • properties of individual source classes • shape of the radio spectra → complete SEDs • correlation between different frequencies • variability at several timescales • modelling of radio sources • ... • Planck data catalogs

  8. Quick Detection System (QDS) • Software package that detects unusual point sources in the time-ordered datastream of Planck in one or two weeks from the initial observation • almost realtime follow-up with other instruments

  9. QDS parameters Emphasis mostly on “surprising” events & sources 1. New flaring objects Includes objects that are expected to be very faint, for example, XBLs, TeV sources etc 2. Inverted spectrum-sources 3. Fast events 4. Strong events in well-known sources

  10. Planck WGs and CTs • Working Groups (science programme) • WG 6 Extragalactic point sources (AGNs) • WG 7 Galactic sources (microquasars, stellar evolution) • Core Teams (all practical work during mission) • CTA-09 Non-CMB science

  11. Planck Baseline Core Science Programme (2001) • The Astrophysics of Quasars and BL Lac Objects • + 4 others including GPS sources, statistical properties, follow-up etc • The Final Planck Science Programme will be defined in 2008 ”The Bluebook” CLASSIFIED

  12. Work @ Metsähovi • Before mission (19992008) • mapping, analysis & modelling of foreground sources (BL Lac & GPS objects, faint quasars, variability) + Pre-launch catalogs  dedicated source samples collected and observed at Metsähovi contain hundreds of sources • simulations, methods, tools, QDS • During mission (20092011) • foreground mapping continues, follow-up observations from ground & with satellites, QDS software operations, publication of QDS results • After mission (2011 ) • Analysis, research and publication of Planck results, follow-up observations

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