Integrated Large Infrastructure for Astroparticle Science

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Integrated Large Infrastructure for
Astroparticle Science

• Geppo CagnoliUniversity of Glasgow andINFN
  Sez. di Firenze
• JENAM Liege 6th July 2005

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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)

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ILIAS Mission

• Support and coordinate a common European Research
  Activity in the strategic areas of
• Double Beta Decay,
• Dark Matter and
• Gravitational Wave Detection

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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

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ILIAS Coordination Managing Scheme
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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
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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

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WIMP Detection

• A challenge!
• ? Weak and gravitational interactions only
• ? Interaction rate events/kg/yr
• (hence background rates crucial)
• ? Small signals
• Mass 11000 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

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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
Diurnal signature - goes in and out of phase with
solar day-night cycle. Directional asymmetry 50
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Direct DMD Search Situation
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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

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Gravitational Wave Detectiona New Astronomy

• 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

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Typical signal strengthof 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



h
Hz 1/2
NS-NS Virgo cluster
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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

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Present situation
VIRGO is about 2 years behind LIGO An array of
detectors isbeing formed
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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



h
Hz 1/2
NS-NS 350Mpc 3/yr 4/day
NS-BH 750Mpc 1/yr 6/day
BH-BH Z0.45 1/month 30/day
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Preparing the Future3rd 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)

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Detection range on NS-NS binaries
1st generation
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Gravitational Wave Research in ILIAS

• Study of Thermal noise Reduction for European
  Gravitational wAve detectors (RD)
• 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

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The activities in STREGA

• 3 Objectives Materials, Cryogenics, Th. Noise
  Selected topics

T1 - Direct ThNsmeasurement facility
T2 - Dynamicphoto-elasticeffect
T3 - Selectiveread-outfor resonators
C1 - Cryogenictop suspensionsfor IFOs
C2 - Cryogenicsystem forresonators
C3 - IFOs last stage suspensions
M1Mirrorsubstrates M2Materials forresonators
M3 Super conductiveRF cavities M4Mirrorcoatings
M5Mirrorsuspensions M6 Cosmic Raysacoustic em.
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Working groups in GWA
A Europeanstrategy forfuture detectors
Antenna commissioning and characterization
Joint operation of antennas and network
dataanalysis
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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/