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

2. The context around ILIAS
ILIAS is an EU project funded under the Framework Program 6
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

3. 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

4. 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

5. 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

6. 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

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 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

8. 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

9. 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

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

11. 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

12. 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

13. 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

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
6th July 2005
JENAM - Liege - G.Cagnoli

15. 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

16. 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

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

18. 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

19. 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

20. 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

21. 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

22. 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
6th July 2005
JENAM - Liege - G.Cagnoli