1 New suspension study for LCGT Erina Nishida Ochanomizu University The Graduate School of Humanities and Sciences The Division of Advanced Sciences/ NAOJ.

Slides:



Advertisements
Similar presentations
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
Advertisements

Participants: C-1:Cryogenic last-stage suspensions (interferometers) (F.Ricci-G.Frossati) Objectives: -Design new suspension elements for the last stage.
1 Test Mass Suspensions for AIGO Ben Lee The University of Western Australia.
Aspects of Fused Silica Suspensions in Advanced Detectors Geppo Cagnoli University of Texas at Brownsville and TSC LIGO, Hanford.
LCGT seismic Attenuation System DRADF DRAFT DRAFT DRAFT.
Generation of squeezed states using radiation pressure effects David Ottaway – for Nergis Mavalvala Australia-Italy Workshop October 2005.
GWADW 2010 in Kyoto, May 19, Development for Observation and Reduction of Radiation Pressure Noise T. Mori, S. Ballmer, K. Agatsuma, S. Sakata,
Cryogenics for LCGT Technical Advisory Committee for LCGT ICRR SUZUKI, Toshikazu High Energy Accelerator Research Organization.
Status of LCGT and CLIO Masatake Ohashi (ICRR, The University of TOKYO) and LCGT, CLIO collaborators TAUP2007 Sendai, Japan 2007/9/12.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
Composite mirror suspensions development status Riccardo DeSalvo For the ELiTES R&D group WP1 & 2 JGW-xxxxxx.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Louisiana,
Conceptual Design for Advanced LIGO Suspensions Norna A Robertson University of Glasgow and Stanford University for the GEO suspension team +contribution.
Australia-Italy Australia 6, October 2005 LCGT project Kazuaki Kuroda LCGT Collaboration Cryogenics for LCGT.
T Akutsu 1, S Telada 2, T Uchiyama 1, S Miyoki 1, K Yamamoto 1, M Ohashi 1, K Kuroda 1, N Kanda 3 and CLIO Collaboration. 1 ICRR, Univ. of Tokyo, 2 AIST,
Composite mirror suspensions development status and directions ELiTES activity interim report JGW-G
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.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Hanford.
Simulation for KAGRA cryogenic payload: vibration via heat links and thermal noise Univ. Tokyo, D1 Takanori Sekiguchi.
LIGO Surf Project Q Of the Thermal Noise Interferometer Adam Bushmaker Mentor: Dr. Eric Black LIGO-G D.
18 th - 22 nd May 2015 LIGO-G GWADW Alaska Suspension Upgrades for Enhanced Interferometers Giles Hammond (Institute for Gravitational Research,
LCGT Technical Review Suspension Point Interferometer for Parasitic Noise Reduction and an Additional IFO S.Miyoki (ICRR, Univ. of TOKYO)
Bridging the Gap between Terrestrial Detectors and LISA Elba 2002 May 24, 2002 Seiji Kawamura National Astronomical Observatory of Japan.
External forces from heat links in cryogenic suspensions D1, ICRR, Univ. Tokyo Takanori Sekiguchi GWADW in Hawaii.
Cold damping of fused silica suspension violin modes V.P.Mitrofanov, K.V.Tokmakov Moscow State University G Z.
Update on Activities in Suspensions for Advanced LIGO Norna A Robertson University of Glasgow and Stanford University LSC meeting, Hanford, Aug 20 th 2002.
Thermal Noise performance of advanced gravitational wave detector suspensions Alan Cumming, on behalf of the University of Glasgow Suspension Team 5 th.
State College May 2004 LIGO- Mining for IMBH Gravitational Waves Fabrizio Barone Enrico Campagna Yanbei Chen Giancarlo Cella Riccardo DeSalvo Seiji Kawamura.
DECIGO – Japanese Space Gravitational Wave Detector International Workshop on GPS Meteorology January 17, Tsukuba Center for Institutes Seiji Kawamura*
Cryogenic Xylophone Kyoto May Kentaro Somiya Waseda Inst. for Adv. Study Collaboration work with S.Hild, K.Kokeyama, H.Mueller-Ebhardt, R.Nawrodt,
Dangers of controls from the cryogenic links. The LCGT-SAS Seismic Attenuation System i-LCGT is a modern, simplified and improved version of the Virgo.
Advanced LIGO UK 1 LIGO-G Z Development issues for the UK Advanced LIGO project Caroline Cantley Glasgow University for the UK Advanced LIGO Team.
2009/6/25Amaldi 8 in NewYork City1 Thermal-noise-limited underground interferometer CLIO Kazuhiro Agatsuma and CLIO Collaborators Institute for Cosmic.
External forces from heat links in cryogenic suspensions D1, ICRR, Univ. Tokyo Takanori Sekiguchi.
LIGO-G Z March 2007, LSC meeting, Osamu Miyakawa 1 Osamu Miyakawa Hiroaki Yamamoto March 21, 2006 LSC meeting Modeling of AdLIGO arm lock acquisition.
111 Kazuhiro Yamamoto Institute for Cosmic Ray Research, the University of Tokyo Cryogenic interferometer technologies 19 May 2014 Gravitational Wave Advanced.
Deci-hertz Interferometer Gravitational Wave Observatory (DECIGO) 7th Gravitational Wave Data Analysis Workshop December 17, International Institute.
Space Gravitational Wave Antenna DECIGO Project 3rd TAMA Symposium February 7, Institute for Cosmic Ray Research, Japan Seiji Kawamura National.
1 Kazuhiro Yamamoto Institute for Cosmic Ray Research The university of Tokyo LCGT internal review (Cryogenic payload) 30 January 2012.
1 Kazuhiro Yamamoto Institute for Cosmic Ray Research The university of Tokyo LCGT internal review (Cryogenic payload) 30 January 2012.
LIGO-G D Advanced LIGO Systems & Interferometer Sensing & Control (ISC) Peter Fritschel, LIGO MIT PAC 12 Meeting, 27 June 2002.
Yoichi Aso Columbia University, New York, NY, USA University of Tokyo, Tokyo, Japan July 14th th Edoardo Amaldi Conference on Gravitational Waves.
Metallurgha.ir1. Lecture 5 Advanced Topics II Signal, Noise and Bandwidth. Fundamental Limitations of force measurement metallurgha.ir2.
Overview of the 20K configuration
New suspension study for LCGT
Pros and cons of cryogenics for Einstein Telescope and Cosmic Explorer
Optimization of thermal noise for ET-LF sensitivity
Progress on Acoustic Mode Damper design
Is there a future for LIGO underground?
Generation of squeezed states using radiation pressure effects
Yoichi Aso on behalf of the LCGT ISC Group
External forces from heat links in cryogenic suspensions
Superattenuator for LF and HF interferometers
Cryogenic Payload Modeling: Vibration via Heat Links
Design of Stable Power-Recycling Cavities
Quantum effects in Gravitational-wave Interferometers
Searching for Excess Noise in Suspensions
1/10 prototype support tube
Flat-Top Beam Profile Cavity Prototype: design and preliminary tests
KAGRA+ Upgrade Plans Yuta Michimura1, Kentaro Komori1
Test Mass Suspensions for AIGO
Searching for Excess Noise in Suspensions
Summary of Issues for KAGRA+
New suspension study for LCGT
Flat-Top Beam Profile Cavity Prototype
Development of vibration isolation systems for LCGT VI
Cryogenic Suspension for KAGRA and Suspension Thermal Noise Issues
CLIO underground in mine
Cryogenic Payload Modeling: Vibration via Heat Links
Presentation transcript:

1 New suspension study for LCGT Erina Nishida Ochanomizu University The Graduate School of Humanities and Sciences The Division of Advanced Sciences/ NAOJ

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 2 LCGT Sensitivity There is a peak at 117Hz Those depends on the fiber being thick and tunnel tilting. bLCGT default parameters Arm length: 3000[m] Test mass: 30[kg] Mass temperature: 20[K] Suspension length: 0.3[m]

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 3 troublesome peak from data analysis One of problem for data analysis is vertical mode at 117Hz LIGO mode frequency is about 300 ~ 400Hz. Sensitivity is worse.( lower S/N→lower detection efficiency) Power is unstable. (power fluctuation make detection efficiency worse) It is difficult to analyze this frequency band. Frequency band this mode could be widen. >> Laser amplitude noise, seismic noise, 4 wires…

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 4 Simulation model Mathmatica Model parameters ●4 sapphire suspensions ●0.30 m length ● 30kg mass fiberribbon

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 5 Why fiber is not effective?? Physics Letters A 270 (2000) ‘Ribbon’ thickness could be thinner while the heat transportation keep. Mechanical lossΦ

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 6 Moving 120Hz peak by changing the fiber shape Including cooling effect, those peaks doesn’t move to lower. Without thermal noise increasing, how to make the peak decrease….is Ribbon, which could make cross section larger, then resonant frequency higher.

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 7 Ribbon cross section constant Ribbon thickness h, width w Cooling effect above 0.8W Comparison of different ribbon ratio Thin ribbon can make violin mode move to higher. Thinner ribbon make 2 nd mode To 500Hz!!

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 8 Ribbon width constant Ribbon thickness h Cooling effect above 0.8W Comparison of different cross sections Vertical mode and violin mode move to higher according to the thickness. 7times area make 1 st mode to 300Hz Those parameters are realistic!!

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 9 VSPI for vertical mode Vertical mode could be suppressed by VSPI. Resonant frequency can be changed. Thermal noise can be reduced. Feedback control [Vertical Suspension Point Interferometer] Alternative solution to reduce vertical TN

LCGT f2f university, Japan, 5th Aug, 2011 Erina Nishida 10 Options for solutions To avoid the suspension peak at the117Hz →Use ribbon which has wide width and thin thickness To avoid vertical mode →vertical SPI Thank you for your attentions!!