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Integrated Large Infrastructure for Astroparticle Science
Geppo Cagnoli
University of Glasgow andINFN Sez. di Firenze
JENAM – Liege – 6th July 2005
6th July 2005 JENAM - Liege - G.Cagnoli 2 of 22
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 3 of 22
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 of 22
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 of 22
ILIAS Coordination Managing Scheme
Steering Committee
SC
Peer Review Committee
PRC
Executive BoardEB
Management TeamMT
European CommissionEC
Coordinator
Governing CouncilGC
Underground LabsCo-ordination &
Management CommitteeDUSL-CoMag
Steering Committee
SC
Peer Review Committee
PRC
Executive BoardEB
Management TeamMT
European CommissionEC
Coordinator
Governing CouncilGC
Governing CouncilGC
Underground LabsCo-ordination &
Management CommitteeDUSL-CoMag
(Contractors)
(Activity Coordinators)
6th July 2005 JENAM - Liege - G.Cagnoli 6 of 22
ILIAS Activities
Coordination and Management
Underground Laboratories Gravitational Wave Infrastructures
Low Background Techniques for DUS
Integrated 2 Decay
Thermal Noise reduction in GW DetectorsDeep Underground Science Labs
Search on 2 Decay
Direct Dark Matter Detection
Gravitational Wave Antennae
T
heore
tical A
str
op
art
icle
Ph
ysic
s
Transnational Access
6th July 2005 JENAM - Liege - G.Cagnoli 7 of 22
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
6th July 2005 JENAM - Liege - G.Cagnoli 8 of 22
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 of 22
Modulation Signatures
• WIMP halo will manifest itself as a WIMP wind
• A directional detector provides a capability to measure this.
42o
midnight
noon
WIMP Wind
Annual modulation~10% variation in signal
strength
Diurnal signature - goes in and out of phase with solar day-night cycle.Directional asymmetry ~50%
6th July 2005 JENAM - Liege - G.Cagnoli 10 of 22
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
6th July 2005 JENAM - Liege - G.Cagnoli 12 of 22
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
Swift Telescope53s after GRB
6th July 2005 JENAM - Liege - G.Cagnoli 13 of 22
Typical signal strengthof C/O inspirals
1 10 100 1k 10kFrequency [Hz]
10 -22
10 -23
10 -24
10 -25
10 -19
10 -20
10 -21
h
[ H
z –1
/2 ]
Distance Rate
NS-NS 20Mpc1/3000yr
1/3yr
NS-BH 43Mpc1/2500yr
1/2yr
BH-BH 100Mpc1/600yr
3/yr
~10 min~3 sec
~10,000 cycles
GEO600
LIGOVIRGO
AURIGANAUTILUS
Seismic
Thermal noise
Shot noise
NS-NS Virgo cluster
6th July 2005 JENAM - Liege - G.Cagnoli 14 of 22
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 about2 years behind LIGO
An array of detectors isbeing formed
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The 2nd Detectors Generation
1 10 100 1k 10kFrequency [Hz]
10 -22
10 -23
10 -24
10 -25
10 -19
10 -20
10 -21
h
[ H
z –1
/2 ]
ADVANCED LIGO
• Stretching to the very limit the room temperature technology
>10 times total noise reduction
Distance Rate
NS-NS 20Mpc1/3000yr
1/3yr
NS-BH 43Mpc1/2500yr
1/2yr
BH-BH 100Mpc1/600yr
3/yr
NS-NS 350Mpc3/yr
4/day
NS-BH 750Mpc1/yr
6/day
BH-BH Z~0.451/month30/day
6th July 2005 JENAM - Liege - G.Cagnoli 17 of 22
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 of 22
Detection range on NS-NS binaries
GRB050509B
AD LIGO/VIRGO
3rd Generation1st
generation
6th July 2005 JENAM - Liege - G.Cagnoli 19 of 22
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 of 22
The activities in STREGA
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.
T1 - Direct ThNsmeasurement
facility
T2 - Dynamicphoto-elastic
effect
T3 - Selectiveread-out
for resonators
• 3 Objectives: Materials, Cryogenics, Th. Noise Selected topics
6th July 2005 JENAM - Liege - G.Cagnoli 21 of 22
Working groups in GWA
Joint operation ofantennas andnetwork data
analysis
A Europeanstrategy for
future detectors
Antennacommissioning
andcharacterization
6th July 2005 JENAM - Liege - G.Cagnoli 22 of 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/