Integrated Large Infrastructure for Astroparticle Science

Slides:



Advertisements
Similar presentations
Michele Punturo European Gravitational Observatory and INFN-Perugia On behalf of the GW ILIAS-next community Gravitational Wave Network.
Advertisements

 ET is a “design study” supported by the European Commission under the Framework Programme 7 (FP7)  It is a ~3 years project supported by EC with about.
FP7 Design study proposal Michele Punturo Harald Lueck.
and the quest for gravitational waves
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
VIRGO: WHERE WE COME FROM WHERE WE ARE GOING GIOVANNI LOSURDO - INFN Firenze Advanced Virgo Project Leader for the Virgo Collaboration (and the LIGO Scientific.
Palma de Mallorca, October 24th, Summary - FP7 & FP6 - Design Study submitted in FP6 - A Design Study for FP7 - Next steps Raffaele Flaminio EGO.
LIGO-G W Is there a future for LIGO underground? Fred Raab, LIGO Hanford Observatory.
1 Observing the Most Violent Events in the Universe Virgo Barry Barish Director, LIGO Virgo Inauguration 23-July-03 Cascina 2003.
Gravitational-waves: Sources and detection
Towards a Design Study Proposal for a 3rd Generation Interferometric Gravitational- wave Detector Harald Lück London, October 26th 2006.
Gravitational Wave Detectors: new eyes for physics and astronomy Gabriela González Department of Physics and Astronomy Louisiana State University.
FP7 and ILIAS-NEXT Geppo Cagnoli INFN Sez. Firenze University of Glasgow 3 rd ILIAS GW Meeting – 26 th Oct. 2006, ICL.
CHIPP Workshop on Detector R&D June - University of Geneva Common R&D for astroparticle physics: Activities of ApPEC and ASPERA Bernard Revaz and.
Integrated Large Infrastructure for Astroparticle Science Geppo Cagnoli University of Glasgow and INFN Sez. di Firenze JENAM – Liege – 6 th July 2005.
1/25 Current results and future scenarios for gravitational wave’s stochastic background G. Cella – INFN sez. Pisa.
Advanced LIGO: our future in gravitational astronomy K.A. Strain for the LIGO Science Collaboration NAM 2008 LIGO-G K.
1  Goal of ILIAS  Activities of ILIAS, running  Status, 3rd y highlights  “ILIAS next”  Links with others - HEAPNet Integrated Large Infrastructures.
Design study for ET 3rd generation Gravitational Wave Interferometer Work Package 2 Suspension, Thermal noise and Cryogenics Piero Rapagnani
ASPERA Status Astronet GB 20 September 2006 S.Katsanevas CNRS/IN2P3.
Paris, November 5th, ILIAS/N5: The GW antenna network Raffaele Flaminio EGO and LAPP/CNRS Summary - History - GWA Objectives & Contents - Management.
Status of LIGO Data Analysis Gabriela González Department of Physics and Astronomy Louisiana State University for the LIGO Scientific Collaboration Dec.
International Conference on Topics in Astroparticle and Underground Physics (Sept. 11, 2007, Sendai, Japan ) DECIGO Pathfinder Masaki Ando (Department.
1 DUSEL and Gravitational Waves Vuk Mandic University of Minnesota 03/17/08.
LIGO- G D Status of LIGO Stan Whitcomb ACIGA Workshop 21 April 2004.
Lisbon, 8 January Research and Development for Gravitational Wave Detectors Raffaele Flaminio CNRS/LMA Lyon.
JRA3 STREGA - Introduction Geppo Cagnoli IGR – University of Glasgow ILIAS-GW Meeting, Orsay, 5 th -6 th Nov 2004.
Advanced interferometers for astronomical observations Lee Samuel Finn Center for Gravitational Wave Physics, Penn State.
1 Gravitational Wave Astronomy using 0.1Hz space laser interferometer Takashi Nakamura GWDAW-8 Milwaukee 2003/12/17.
Silicon as material for 3rd Generation detectors Geppo Cagnoli University of Glasgow INFN Sez. Firenze 2 nd ILIAS-GW Meeting – 25 th Oct. 2005, Palma de.
R&D on thermal noise in Europe: the STREGA Project Geppo Cagnoli University of Glasgow AMALDI 6 – Okinawa - Japan June
A proposal for additional Low Frequency Gravitational Wave Interferometric Detectors at LIGO Riccardo DeSalvo California Institute of Technology Globular.
DECIGO – Japanese Space Gravitational Wave Detector International Workshop on GPS Meteorology January 17, Tsukuba Center for Institutes Seiji Kawamura*
LIGO-G D Upper Limits on the Stochastic Background of Gravitational Waves from LIGO Vuk Mandic Einstein2005 Conference Paris, July
Fundamental Physics, Astrophysics and Cosmology with ET p1 Michele Punturo on behalf of the ET team GA # A short introduction to the project.
International Gravitational Wave Network 11/9/2008 Building an Stefan Ballmer, for the LIGO / VIRGO Scientific Collaboration LIGO G
ILIAS Project Summary ILIAS is an Integrated Infrastructure Initiative that has pulled together all of Europe's leading infrastructures in Astroparticle.
LIGO-G M Press Conference Scientific Operation of LIGO Gary H Sanders Caltech (on behalf of a large team) APS April Meeting Philadelphia 6-April-03.
Space Gravitational Wave Antenna DECIGO Project 3rd TAMA Symposium February 7, Institute for Cosmic Ray Research, Japan Seiji Kawamura National.
Michele Punturo INFN Perugia and EGO 11st ELiTES meeting.
Gravitational Wave Physics Programme: - new initiative - Group composition (current): 3 staff, 0 postdoc, 2 PhD Investment Budget: under discussion Jo.
Harald Lück AEI Hannover. Thank you Science Team! You did a great job!
Michele Punturo EGO & INFN Perugia 1 2nd ET meeting, Erice Oct'09.
THE NEXT GENERATIONS OF GRAVITATIONAL WAVE DETECTORS (*) Giovanni Losurdo INFN Firenze – Virgo collaboration (*) GROUND BASED, INTERFEROMETRIC.
Michele Punturo INFN Perugia and EGO 1MGR13- ET.
Gravitational Waves What are they? How can they be detected?
Gravitational Wave Astronomy
The Quest for Gravitational Waves: a global strategy
Brennan Hughey MIT Kavli Institute Postdoc Symposium
Critical Technology Giant leaps Near-term steps Non-IFO methods
Current and future ground-based gravitational-wave detectors
GW Policy: The Future: G3 Detectors
Dark Matter Search With an Ultra-low Threshold Germanium Detector proposed by Tsinghua University Seoul National University Academia Sinica Qian Yue.
DECIGO Pathfinder Masaki Ando
THE NEXT GENERATION OF GRAVITATIONAL WAVE DETECTORS
Commission II meeting – 7 March 2009
Astrophysics: 2016 highlights and the way forward
Is there a future for LIGO underground?
Advanced VIRGO Experiment
LIGO detectors: past, present and future
GW150914: The first direct detection of gravitational waves
Gravitational wave detection and the quantum limit
2nd ILIAS-GW Meeting – 25th Oct. 2005, Palma de Mallorca
Jim Hough for the GEO collaboration
WP4 Positioning European Astroparticle Physics in the world-wide context WP leader CNRS Partners: FOM, IFIN-HH, FRS-FNRS/FWO, FCT Total work: 22 months.
Update on Status of LIGO
Detection of Gravitational Waves with Interferometers
P Fritschel LSC Meeting LLO, 22 March 2005
The views of Virgo collaboration groups on upgraded/advanced Virgo
The Estimated Limits For A 5g LE-Ge Detector
Presentation transcript:

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