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ASPERA Status

per aspera ad astra. AStroparticle ERAnet. ASPERA Status. Astronet GB 20 September 2006 S.Katsanevas CNRS/IN2P3. What is the AstroParticle ERA net (ASPERA)?. An EU ERANET program with

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ASPERA Status

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  1. per aspera ad astra AStroparticle ERAnet ASPERA Status Astronet GB 20 September 2006 S.Katsanevas CNRS/IN2P3

  2. What is the AstroParticle ERA net (ASPERA)? • An EU ERANET program with • 17 partners from 12 countries and CERN, CNRS coordinator, ambition to cover all countries with astroparticle activities in Europe • EU budget 2.5 M€ for 3 years (1 July 2006 to 1 July 2009) used for 33 meetings, 10 new liaison officers , 26 deliverables, 5 milestones. • Goals (increasing level of ambition) • Evaluate the current status of Astroparticle Physics funding in Europe • Provide the community with a common electronic infrastructure and outreach policy • Increase the partnership to all European countries with activities in Astroparticle, coordinate with other regions • Prepare a detailed roadmap and strategic plan of the facilities • Propose common evaluation procedures, management, benchmarks • Achieve integration/coordination/linking of facilities (Ulabs, CT, GWA) • Achieve common funding calls (e.g for R&D) • Achieve partial alignment of funds in Europe for Astroparticle

  3. ASPERA 17 agencies 12 countries + CERN: Belgium FNRS/FWO Czech Rep. MEYS France CEA/CNRS Germany BMBF/PTDESY Greece DEMOKRITOS Italy INFN Netherlands FOM Portugal FCT Spain MEC/FECYT Sweden VR Switzerland SNF UK PPARC CERN

  4. WP3 European wide procedures INFN 5 workpackages WP1 Status in research funding NIKHEF WP2 Roadmap PPARC WP4 Web/Database/Outreach Network Extension BMBF/MEC WP5 Management CNRS

  5. Management structure

  6. ASPERA WP1 Status APP funding in Europe Inventory of systems & rules Identify barriers for collaboration (legal, financial)

  7. Collect status information • How do other agencies operate • Funding philosophy • Which programs? • Who can be funded? • Which disciplines? • Conditions? • Other organisations? WP 1

  8. Instruments • Program manager meetings: • Define criteria (early 2007) 1st workshop 15 January 2007 Paris • Working stays abroad: Administrative open days • a.1st meeting in Paris on the 16/17 of January 2007 in Paris • b. 2nd meeting April in Amsterdam • c. 3rd meeting June in Hambourg • d. 4th meeting July London • e. 5th meeting October Rome • f. 6th meeting November Madrid • g. 7th meeting January 2008 Geneva/Bern • h. 8th meeting March Brussels • i. 9th meeting May Lisbon • j. 10th meeting June Stockholm • k. 11th meeting September Athens • 12th meeting November Prague • A draft document ready a few major agencies serve as “cobays” for its pertinence before large diffusion (PPARC,INFN,CNRS,INFN, FOM)

  9. ASPERA WP2 A Roadmap for APP in Europe Roadmap and areas of common R&D Formulation of a common evaluation policy A posteriori linking of existing infrastructures

  10. Astroparticle Physics, a definition through 6 questions* Courtesy ApPEC PRC • What is the Universe made of ? • Do protons have a finite life time ? • What are the properties of neutrinos ? What is their role in cosmic evolution ? • What do neutrinos tell us about the interior of Sun and Earth, and about Supernova explosions ? • What is the origin of cosmic rays ? What is the view of the sky at extreme energies ? • What is the nature of gravity ? Can we detect gravitational waves ? What will they tell us about violent cosmic processes ? *”Science is the art of replacing unimportant questions that can be answered by important ones which cannot” Edward B. Ferguson Jr. 1976.

  11. A definition through instruments • High Energy neutrinos • High energy gamma rays • Gravitational antennas • High energy cosmic rays • Dark matter • Large Underground Detectors • Neutrinos mass (endpoint, doublebeta) and reactor neutrinos

  12. satellite MeV/GeV  (Agile, Glast) MeV/GeV CR (Pamela, AMS) CR @ extreme energies Charged Cosmic Rays GeV-TeV gamma (incl. DM indirect) WIMP Solar axions CAST i.e. Hess, Auger UG lab underwater underice UG lab DM direct HE neutrinos atm. neutrinos (incl. DM indirect) Solar  Supernova  Spiering, ApPEC.

  13. m Laser axions Reactor Accelerator Oscillations (accelerators)  NO proton decay • No particles from heaven but: • - same infrastructure () • closely related question (tritium decay) NO UG lab  Spiering, ApPEC.

  14. Interferometer low frequency (LISA) Gravitational Waves Interferometers (Geo-600, VIRGO) Resonance Antennas Spiering, ApPEC.

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