Integrated Large Infrastructure for Astroparticle Science Geppo Cagnoli University of Glasgow and INFN Sez. di Firenze JENAM – Liege – 6th July 2005

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) 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli ILIAS Mission Support and coordinate a common European Research Activity in the strategic areas of Double Beta Decay, Dark Matter and Gravitational Wave Detection 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli 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€ 6th July 2005 JENAM - Liege - G.Cagnoli

ILIAS Coordination Managing Scheme Steering Committee SC Peer Review PRC Executive Board EB Management Team MT European Commission EC Coordinator Governing Council GC Underground Labs Co - ordination & Management DUSL CoMag (Contractors) (Activity Coordinators) 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli ILIAS Activities Coordination and Management Underground Laboratories Gravitational Wave Infrastructures 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 6th July 2005 JENAM - Liege - G.Cagnoli

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 pb i.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 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli 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 6th July 2005 JENAM - Liege - G.Cagnoli

Modulation Signatures 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 42o midnight noon WIMP Wind Diurnal signature - goes in and out of phase with solar day-night cycle. Directional asymmetry ~50% 6th July 2005 JENAM - Liege - G.Cagnoli

Direct DMD Search Situation 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli 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 6th July 2005 JENAM - Liege - G.Cagnoli

Gravitational Wave Detection a New Astronomy Gravitational Waves are precursors of the most violent events in the Universe GRB050509B Swift Telescope 53s after GRB Merging of Compact Objects, Pulsars, SN explosions, Cosmic Strings and Dark Matter can be investigated with GW The effect of GW is pure mechanical 6th July 2005 JENAM - Liege - G.Cagnoli

Typical signal strength of C/O inspirals Distance Rate NS-NS 20Mpc 1/3000yr 1/3yr NS-BH 43Mpc 1/2500yr 1/2yr BH-BH 100Mpc 1/600yr 3/yr 1 10 100 1k 10k Frequency [Hz] GEO600 LIGO VIRGO AURIGA NAUTILUS Seismic Thermal noise 10 -22 10 -23 10 -24 10 -25 10 -19 10 -20 10 -21 Shot noise h ~10 min ~3 sec ~10,000 cycles [ Hz –1/2 ] NS-NS Virgo cluster 6th July 2005 JENAM - Liege - G.Cagnoli

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 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli Present situation VIRGO is about 2 years behind LIGO An array of detectors is being formed 6th July 2005 JENAM - Liege - G.Cagnoli

The 2nd Detectors Generation Distance Rate NS-NS 20Mpc 1/3000yr 1/3yr NS-BH 43Mpc 1/2500yr 1/2yr BH-BH 100Mpc 1/600yr 3/yr 1 10 100 1k 10k Frequency [Hz] ADVANCED LIGO Stretching to the very limit the room temperature technology >10 times total noise reduction 10 -22 10 -23 10 -24 10 -25 10 -19 10 -20 10 -21 h [ Hz –1/2 ] NS-NS 350Mpc 3/yr 4/day NS-BH 750Mpc 1/yr 6/day BH-BH Z~0.45 1/month 30/day 6th July 2005 JENAM - Liege - G.Cagnoli

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) 6th July 2005 JENAM - Liege - G.Cagnoli

Detection range on NS-NS binaries 3rd Generation Detection range on NS-NS binaries GRB050509B AD LIGO/VIRGO 1st generation 6th July 2005 JENAM - Liege - G.Cagnoli

Gravitational Wave Research in ILIAS Study of Thermal noise Reduction for European Gravitational wAve detectors (R&D) Gravitational Wave Antennae (Networking) STREGA mission Lower thermal noise 10 times with respect to the second 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 6th July 2005 JENAM - Liege - G.Cagnoli

The activities in STREGA 3 Objectives: Materials, Cryogenics, Th. Noise Selected topics M1 Mirror substrates M2 Materials for resonators M3 – Super conductive RF cavities M4 Mirror coatings M5 Mirror suspensions M6 Cosmic Rays acoustic em. C1 - Cryogenic top suspensions for IFOs C2 - Cryogenic system for resonators C3 - IFOs last stage suspensions T1 - Direct ThNs measurement facility T2 - Dynamic photo-elastic effect T3 - Selective read-out for resonators 6th July 2005 JENAM - Liege - G.Cagnoli

Working groups in GWA Antenna Joint operation of commissioning and characterization Joint operation of antennas and network data analysis A European strategy for future detectors 6th July 2005 JENAM - Liege - G.Cagnoli

JENAM - Liege - G.Cagnoli Conclusion First of the 5 years is already concluded 1st year report is being assessed by the EC All the deliverables (mostly reports) have been successfully 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/ 6th July 2005 JENAM - Liege - G.Cagnoli