Integrated Large Infrastructure for Astroparticle Science

Geppo Cagnoli

University 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

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)

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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

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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 ~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

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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%

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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

Swift Telescope53s after GRB

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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

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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 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

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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)

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Detection range on NS-NS binaries

GRB050509B

AD LIGO/VIRGO

3rd Generation1st

generation

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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

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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

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Working groups in GWA

Joint operation ofantennas andnetwork data

analysis

A Europeanstrategy for

future detectors

Antennacommissioning

andcharacterization

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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/