Some ideas on advanced Virgo Twins A. Giazotto-INFN Pisa

Slides:



Advertisements
Similar presentations
Stray Light Control & Viewports Michael Smith aLIGO NSF Review LIGO Livingston Observatory April LIGO-G v3.
Advertisements

Some ideas on ET1 site Adalberto Giazotto INFN Pisa- EGO.
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
LIGO-G v2 Form F v1 Advanced LIGO1 SCATTERED LIGHT CONTROL in ADVANCED LIGO Michael Smith LIGO Laboratory Caltech, Pasadena, CA.
LIGO-G M First Generation Interferometers Barry Barish 30 Oct 2000 Workshop on Astrophysical Sources for Ground-Based Gravitational Wave Detectors.
Design study for 3rd generation interferometers Work Package 1 Site Identification Jo van den Brand
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
1 Science Opportunities for Australia Advanced LIGO Barry Barish Director, LIGO Canberra, Australia 16-Sept-03 LIGO-G M.
LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
LIGO-G W Is there a future for LIGO underground? Fred Raab, LIGO Hanford Observatory.
LIGO-G9900XX-00-M LIGO Status and Plans Barry Barish 5 June 2000 Gravitational Waves: A Challenge to Theoretical Astrophysics Trieste, 5-9 June 2000.
Status of the LIGO Project
LIGO-G9900XX-00-M LIGO: Progress and Prospects Barry Barish 18 July 2000 COSPAR 2000 Fundamental Physics in Space.
LIGO-G9900XX-00-M LIGO Status and Plans Barry Barish March 13, 2000.
Overview Ground-based Interferometers Barry Barish Caltech Amaldi-6 20-June-05.
G M LIGO Laboratory1 Overview of Advanced LIGO David Shoemaker PAC meeting, NSF Review 5 June 2003, 11 June 2003.
TeV Particle Astrophysics August 2006 Caltech Australian National University Universitat Hannover/AEI LIGO Scientific Collaboration MIT Corbitt, Goda,
Generation of squeezed states using radiation pressure effects David Ottaway – for Nergis Mavalvala Australia-Italy Workshop October 2005.
Virgo Control Noise Reduction
LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
1/25 Current results and future scenarios for gravitational wave’s stochastic background G. Cella – INFN sez. Pisa.
The GEO 600 Detector Andreas Freise for the GEO 600 Team Max-Planck-Institute for Gravitational Physics University of Hannover May 20, 2002.
LIGO- G D Status of LIGO Stan Whitcomb ACIGA Workshop 21 April 2004.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v1.
LIGO-G D The LIGO-I Gravitational-wave Detectors Stan Whitcomb CaJAGWR Seminar February 16, 2001.
LIGO- G D The LIGO Instruments Stan Whitcomb NSB Meeting LIGO Livingston Observatory 4 February 2004.
Gravitational Wave Detection Using Precision Interferometry Gregory Harry Massachusetts Institute of Technology - On Behalf of the LIGO Science Collaboration.
LIGO-G M Major International Collaboration in Advanced LIGO R&D Gary Sanders NSF Operations Review Hanford February, 2001.
1 Virgo Commissioning progress ILIAS, Nov 13 th 2006 Matteo Barsuglia on behalf of the Commissioning Team.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
1 The Virgo noise budget Romain Gouaty For the Virgo collaboration GWADW 2006, Isola d’Elba.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
Cascina, June 19th, Brewster window noise ? Raffaele Flaminio EGO and CNRS/LAPP Summary - Original observations - Brewster window replacement - New.
Status of VIRGO Lisa Barsotti - University and INFN Pisa – on behalf of the VIRGO collaboration ANNECY - December 15 th, 2004  Status of the Commissioning.
Nov 3, 2008 Detection System for AdV 1/8 Detection (DET) Subsystem for AdV  Main tasks and requirements for the subsystem  DC readout  Design for: the.
DECIGO – Japanese Space Gravitational Wave Detector International Workshop on GPS Meteorology January 17, Tsukuba Center for Institutes Seiji Kawamura*
LIGO-G D LIGO Laboratory1 Stoyan Nikolov LIGO-G D The LIGO project’s quest for gravitational waves Presenting LIGO to the students of.
1 Virgo Commissioning Status WG1 meeting Potsdam, 21 st July 2006.
LIGO-G D Upper Limits on the Stochastic Background of Gravitational Waves from LIGO Vuk Mandic Einstein2005 Conference Paris, July
Paolo La Penna ILIAS N5-WP1 meeting Commissioning Progress Hannover, July 2004 VIRGO commissioning progress report.
International Gravitational Wave Network 11/9/2008 Building an Stefan Ballmer, for the LIGO / VIRGO Scientific Collaboration LIGO G
Initial and Advanced LIGO Status Gregory Harry LIGO/MIT March 24, 2006 March 24, th Eastern Gravity Meeting G R.
Optical Spring Experiments With The Glasgow 10m Prototype Interferometer Matt Edgar.
LIGO-G M Scientific Operation of LIGO Gary H Sanders LIGO Laboratory California Institute of Technology APS Meeting APR03, Philadelphia Gravitational-Wave.
Stochastic Background Data Analysis Giancarlo Cella I.N.F.N. Pisa first ENTApP - GWA joint meeting Paris, January 23rd and 24th, 2006 Institute d'Astrophysique.
Caltech, February 12th1 Virgo central interferometer: commissioning and engineering runs Matteo Barsuglia Laboratoire de l’Accelerateur Lineaire, Orsay.
LIGO G M Intro to LIGO Seismic Isolation Pre-bid meeting Gary Sanders LIGO/Caltech Stanford, April 29, 2003.
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.
LIGO-G Z LIGO’s Thermal Noise Interferometer Progress and Status Eric D. Black, Kenneth G. Libbrecht, and Shanti Rao (Caltech) Seiji Kawamura.
Space Gravitational Wave Antenna DECIGO Project 3rd TAMA Symposium February 7, Institute for Cosmic Ray Research, Japan Seiji Kawamura National.
LOGO Gravitational Waves I.S.Jang Introduction Contents ii. Waves in general relativity iii. Gravitational wave detectors.
The quest for gravitational waves. 2 The Universe has been studied essentially through EM radiation. GWs have a different origin. The Scientific Motivation.
MG 11 - Berlin Virgo status Marie-Anne Bizouard (LAL-Orsay) on behalf of the Virgo Collaboration.
Back-scattered light noise in Virgo 2nd Science Run data
Reaching the Advanced LIGO Detector Design Sensitivity
Is there a future for LIGO underground?
Generation of squeezed states using radiation pressure effects
LIGO detectors: past, present and future
Baffle arrangement for LCGT
Nergis Mavalvala MIT IAU214, August 2002
Superattenuator for LF and HF interferometers
Design of Stable Power-Recycling Cavities
Flat-Top Beam Profile Cavity Prototype: design and preliminary tests
Status of LIGO Installation and Commissioning
Albert Lazzarini California Institute of Technology
Improving LIGO’s stability and sensitivity: commissioning examples
Squeezed Light Techniques for Gravitational Wave Detection
Lessons Learned from Commissioning of Advanced Detectors
The views of Virgo collaboration groups on upgraded/advanced Virgo
Advanced Optical Sensing
Presentation transcript:

Some ideas on advanced Virgo Twins A. Giazotto-INFN Pisa If this is true, one appealing idea could be to build a second Virgo:

Some interesting test on twin beams 1)Direct measurement of Scattered Light Effect on the Sensitivity in TAMA300 Ryutaro Takahashi, Koji Arai, Seiji Kawamura and Michael Smith* National Astronomical Observatory of Japan, Caltech*

Experimental method Vibrate the mid point of the arm using a shaker vertically. 5.6 x 10-6m @776.5Hz 4.7 x 10-6m @788.5Hz Measure the effects due to vibration and sound.

Experimental result 1 (signals of the interferometer)

Results and discussion 776.5Hz 788.5Hz Interferometer 1.2 x 10-17m 0.25 x 10-17m (Background) 0.16 x 10-17m 0.13 x 10-17m Vibration  <0.1 x 10-17m <0.01 x 10-17m Sound not detected 0.2 x 10-17m Calculation (with 2-m reflection area and optimal phase) 6.3 x 10-17m There is cancellation due to mechanical modes.

Approximate Conclusions from TAMA TAMA Tube: Diam.~40 cm, No Baffles Vibration TF @ 765 Hz : ~10-17/5 10-6=2 10-12 Scale to Virgo Seismic noise in Virgo is expected to be xVirgo~10-7/2 m/Hz1/2 Expected seismic correlated signal in the two beams~ 2 10-12. 10-7/2= 2 10-19/2 m/Hz1/2 Expected reduction due to Baffles~1/10 ~2 10-20/2 m/Hz1/2

2)Preliminary data from 2km and 4km Hanford ITF’s seems to show low correlation.

From LIGO it seems that: Seismic noise correlate up 30 Hz due to suspensions. Switching power supply create bad correlations at 60 Hz harmonics; needed analog power supply and very good groundings. 3) Sound correlate on injection systems due to common housing.

Virgo seems to have an optimal configuration from three relevant points of views: 1) Very good seismic isolation down to 4Hz 2) Buildings for the second ITF may be completely separated from Virgo 1, this reduces a lot sound and e.m. couplings on the two injection systems. 3) Baffles are installed in the vacuum tube 4) We may also design the overall electronics to be powered with analog Power Supply. 5) A problem: overlapped beams may give coincidences due to dust falling in the vacuum pipe.

VIRGO 2 VIRGO1