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Integrated Large Infrastructure for Astroparticle Science

Integrated Large Infrastructure for Astroparticle Science. Geppo Cagnoli University of Glasgow and INFN Sez. di Firenze JENAM – Liege – 6 th July 2005. The context around ILIAS. ILIAS is an EU project funded under the Framework Program 6 http://ilias.in2p3.fr/

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Integrated Large Infrastructure for Astroparticle Science

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  1. Integrated Large Infrastructure for Astroparticle Science Geppo CagnoliUniversity of Glasgow andINFN Sez. di Firenze JENAM – Liege – 6th July 2005

  2. The context around ILIAS • ILIAS is an EU project funded under the Framework Program 6 http://ilias.in2p3.fr/ • Bijan Saghai from CEA (Saclay)is the coordinator • It has been promoted by ApPEC(Astro-particle Physics European Coordination) JENAM - Liege - G.Cagnoli

  3. ILIAS Mission Support and coordinate a common European Research Activity in the strategic areas of • Double Beta Decay, • Dark Matter and • Gravitational Wave Detection JENAM - Liege - G.Cagnoli

  4. ILIAS summary data • Start: April 1st 2004 • 20 contractors from 12 countries ~ 70 labs • Other contributing labs • 20 countries, 6 outside EU • ~ 70 labs • Budget • 10M€ total • 7.5M€ EC contribution DELIVERABLES • 3 Joint Research Activities 4.1M€ • 5 Networking Activities 2.7M€ • 1 Transnational Access 0.7M€ JENAM - Liege - G.Cagnoli

  5. ILIAS Coordination Managing Scheme European Commission European Commission EC EC Coordinator Coordinator Governing Council Governing Council Governing Council GC (Contractors) GC GC Peer Review Peer Review Steering Steering Committee Committee Committee Committee PRC PRC SC SC Underground Labs Underground Labs Executive Board Executive Board Co Co - - ordination & ordination & EB EB Management Management (Activity Coordinators) Committee Committee DUSL DUSL - - CoMag CoMag Management Team Management Team MT MT JENAM - Liege - G.Cagnoli

  6. ILIAS Activities Coordination and Management Gravitational Wave Infrastructures Underground Laboratories Low Background Techniques for DUS Deep Underground Science Labs Thermal Noise reduction in GW Detectors Gravitational Wave Antennae Integrated 2b Decay Theoretical Astroparticle Physics Search on 2b Decay Direct Dark Matter Detection Transnational Access JENAM - Liege - G.Cagnoli

  7. Direct Dark Matter Detection • Dark Matter issues • Primordial nucleosynthesis and CMB limit the baryonic matter at just 15% of the total • WIMPs are the most likely candidate for the Dark Matter • Next Generation Detectors aim to 10 -10 pbi.e. several 100s kg of target masses + low background • Objectives • Convergence in the assessment of different detector concepts • Convergence on the strategy for future large scale European dark matter experiments JENAM - Liege - G.Cagnoli

  8. WIMP Detection A challenge! Weak and gravitational interactions only  Interaction rate « events/kg/yr (hence background rates crucial) Small signals • Mass ~1–1000 GeV/c2 • Velocity limited by binding to Galaxy  Recoil nuclei: Ekinetic ~few keV Recoil due to neutron difficult to distinguish from WIMP recoil  Expected signal modulations JENAM - Liege - G.Cagnoli

  9. Modulation Signatures noon 42o WIMP Wind midnight • WIMP halo will manifest itself as a WIMP wind • A directional detector provides a capability to measure this. Annual modulation ~10% variation in signal strength Diurnal signature - goes in and out of phase with solar day-night cycle. Directional asymmetry ~50% JENAM - Liege - G.Cagnoli

  10. Direct DMD Search Situation JENAM - Liege - G.Cagnoli

  11. Direct DMD Working Groups(Josef Jochum, Uni. of Tübingen, coordinator) Detection Techniques Cryogenic Detectors and Cryostat Liquid Xenon Detectors Ge and NaI Detectors Advanced Detectors including directional concepts Common Issues Background Simulation and Neutron Shielding High Purity Materials and Purification Techniques Axion Search Common theoretical aspects JENAM - Liege - G.Cagnoli

  12. Gravitational Wave Detectiona New Astronomy Swift Telescope53s after GRB • Gravitational Waves are precursors of the most violent events in the Universe • GRB050509B • Merging of Compact Objects, Pulsars, SN explosions, Cosmic Strings and Dark Matter can be investigated with GW • The effect of GW is pure mechanical JENAM - Liege - G.Cagnoli

  13. Typical signal strengthof C/O inspirals LIGO Seismic VIRGO 10 -19 Thermal noise AURIGA NAUTILUS Shot noise 10 -20 GEO600 ~10 min 10 -21 ~3 sec 10 -22 10 -23 10 -24 ~10,000 cycles 10 -25 10 100 1k 10k 1 Frequency [Hz] h [ Hz –1/2 ] NS-NS Virgo cluster JENAM - Liege - G.Cagnoli

  14. Thermal noise limit to the GW detection All the Earth based detectors are limited by thermal noise that causes fluctuations on position and shape of the test masses • Interferometers: thermal noise in mirrors and in suspension fibres • Bars/Spheres: thermal noise in the resonant elements JENAM - Liege - G.Cagnoli

  15. Present situation VIRGO is about 2 years behind LIGO An array of detectors isbeing formed JENAM - Liege - G.Cagnoli

  16. The 2nd Detectors Generation • Stretching to the very limit the room temperature technology • >10 times total noise reduction 10 -19 10 -20 10 -21 10 -22 ADVANCED LIGO 10 -23 10 -24 10 -25 10 100 1k 10k 1 Frequency [Hz] h [ Hz –1/2 ] JENAM - Liege - G.Cagnoli

  17. Preparing the Future:3rd Generation of Detectors • The Advanced Detectors will stretch to the very limit the room temperature technology for interferometers • Any minimal change of the specs has great effect in the detection distance • We have to secure the detection distance and potentially increase it with a further 10 times reduction of the detector noise • Low temperature is the most promising direction • Japan has already started the design of the LCGT (Large Cryogenic Gravitational Telescope) • Complementary to LISA (Space borne interferometer) JENAM - Liege - G.Cagnoli

  18. Detection range on NS-NS binaries GRB050509B 3rd Generation AD LIGO/VIRGO 1stgeneration JENAM - Liege - G.Cagnoli

  19. Gravitational Wave Research in ILIAS • Study of Thermal noise Reduction forEuropean Gravitational wAve detectors (R&D) • Gravitational Wave Antennae (Networking) • STREGA mission • Lower thermal noise 10 times with respect to thesecond generation detectors • STREGA coordinates the efforts that many labs in different projects spend on Thermal Noise Research • GWA facilitates the collaboration between the different detectors JENAM - Liege - G.Cagnoli

  20. The activities in STREGA • 3 Objectives: Materials, Cryogenics, Th. Noise Selected topics JENAM - Liege - G.Cagnoli

  21. Working groups in GWA Antenna commissioning and characterization A Europeanstrategy forfuture detectors Joint operation of antennas and network dataanalysis JENAM - Liege - G.Cagnoli

  22. Conclusion • First of the 5 years is already concluded • 1st year report is being assessed by the EC • All the deliverables (mostly reports) have beensuccessfully produced • The coordination across labs of different projects is satisfactory • ILIAS is planning already to extend its activity to the next FP7 • More details in http://ilias.in2p3.fr/ JENAM - Liege - G.Cagnoli

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