Participants: C-1:Cryogenic last-stage suspensions (interferometers) (F.Ricci-G.Frossati) Objectives: -Design new suspension elements for the last stage.

Slides:



Advertisements
Similar presentations
STREGA C1:Cryogenic Last Stage Suspension (10 MIN) Task -C1: thermal conduction investigation of final stage suspension; This part of the suspension system.
Advertisements

Piero Rapagnani I.N.F.N. Sezione di Roma
STREGA C2:Cryogenic suspension system for advanced resonant detectors (5 MIN) Task -C2: development and construction of advanced cryogenic system for resonant.
Lecture Notes Part 4 ET 483b Sequential Control and Data Acquisition
Task M2 – Advanced Materials and Techniques for Resonant Detectors Motivation : Reduce thermal noise contribution to the acoustic detector noise budget.
Design and performance of the Dual detector with large area capacitive readout 4 rd ILIAS-GW Meeting, October 8 th – 9 th 2007, Tuebingen Paolo Falferi.
Nawrodt 10/07 #1/21 R. Nawrodt, A. Schröter, C. Schwarz, D. Heinert, M. Hudl, W. Vodel, A. Tünnermann, P. Seidel STREGA Meeting Tübingen 10/
The Use of Small Coolers for Hydrogen and Helium Liquefaction
Acoustic properties of a prototype for a hollow spherical gravitational antenna (^) Laboratori Nazionali del Gran Sasso dell’INFN (*) Laboratori Nazionali.
LIGO-G D Suspensions Update: the View from Caltech Phil Willems LIGO/Caltech Livingston LSC Meeting March 17-20, 2003.
April 27th, 2006 Paola Puppo – INFN Roma ILIAS Cryogenic payloads and cooling systems (towards a third generation interferometer) part II: the Vibration.
1 Update on Focus Coil Design and Configuration M. A. Green, G. Barr, W. Lau, R. S. Senanayake, and S. Q. Yang University of Oxford Department of Physics.
Mechanical amplifiers for the DUAL detector: lumped and distributed element design 3 rd ILIAS-GW Meeting, October 26 th – 27 th 2006, London Paolo Falferi.
ILIAS meeting Mallorca 2005 V. Fafone Viviana Fafone INFN - LNF Future plans for resonant detectors
Active Seismic Isolation Systems for Enhanced and Advanced LIGO Jeffrey S. Kissel 1 for the LSC 1 Louisiana State University The mechanical system for.
1 New suspension study for LCGT Erina Nishida Ochanomizu University The Graduate School of Humanities and Sciences The Division of Advanced Sciences/ NAOJ.
Cryogenics for LCGT Technical Advisory Committee for LCGT ICRR SUZUKI, Toshikazu High Energy Accelerator Research Organization.
ILIAS GW Meeting Mallorca - October 23-24, 2005Luca Taffarello Status of the commissioning of the AURIGA detector Luca Taffarello (INFN Sezione di Padova)
Status of LCGT and CLIO Masatake Ohashi (ICRR, The University of TOKYO) and LCGT, CLIO collaborators TAUP2007 Sendai, Japan 2007/9/12.
Paik-1 Search for Gravitational Waves Ho Jung Paik University of Maryland and Seoul National University January 12, 2006 Seoul, Korea KIAS-SNU Physics.
1 Paolo Falferi - ET WG2 meeting - Glasgow, 22/7/2010 Actuator magnetic noise measurement and possible developments Paolo Falferi CNR-FBK Trento and INFN.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Louisiana,
Design study for ET 3rd generation Gravitational Wave Interferometer Work Package 2 Suspension, Thermal noise and Cryogenics Piero Rapagnani
GWDAW 9 - December 15 th, 2004 STATUS OF EXPLORER AND NAUTILUS INFN – LN Frascati, LN Gran Sasso, Sez. Roma 1, Roma 2 and Genova Universities “La Sapienza”
Australia-Italy Australia 6, October 2005 LCGT project Kazuaki Kuroda LCGT Collaboration Cryogenics for LCGT.
Materials and Cooling Techniques G. Frossati, A.de Waard, L.Gottardi and O.Usenko Kamerlingh Onnes Laboratory Leiden, The Netherlands.
WP1 Teleconference June Luca Taffarello The status report of the AURIGA detector Luca Taffarello (INFN Sezione di Padova ) Special tanks to L. Conti.
HD target.
Ultra-cryogenics for advanced resonant detectors (C2) G.Frossati Kamerlingh Onnes Laboratory Leiden, The Netherlands Second ILIAS-GW Meeting.
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,
JRA3 STREGA - Introduction Geppo Cagnoli IGR – University of Glasgow ILIAS-GW Meeting, Orsay, 5 th -6 th Nov 2004.
SUSPENSION DESIGN FOR ADVANCED LIGO: Update on GEO Activities Norna A Robertson University of Glasgow for the GEO 600 suspension team LSC Meeting, Hanford.
/18 Cryogenic thermometry for refrigerant distribution system of JT-60SA Kyohei NATSUME, Haruyuki MURAKAMI, Kaname KIZU, Kiyoshi YOSHIDA, Yoshihiko KOIDE.
Advanced Virgo Optical Configuration ILIAS-GW, Tübingen Andreas Freise - Conceptual Design -
Simulation for KAGRA cryogenic payload: vibration via heat links and thermal noise Univ. Tokyo, D1 Takanori Sekiguchi.
Task M2 – Working group Auriga-LNL Operation temperature KOperation temperature K Mechanical Attenuation >180dB in the frequency range.
LCGT Technical Review Suspension Point Interferometer for Parasitic Noise Reduction and an Additional IFO S.Miyoki (ICRR, Univ. of TOKYO)
External forces from heat links in cryogenic suspensions D1, ICRR, Univ. Tokyo Takanori Sekiguchi GWADW in Hawaii.
R&D on thermal noise in Europe: the STREGA Project Geppo Cagnoli University of Glasgow AMALDI 6 – Okinawa - Japan June
STREGA-C3 Cryogenic Seismic Isolation Roberto Passaquieti Dipartimento di Fisica “E. Fermi” Università di Pisa INFN sezione di Pisa ILIAS-GW Annual General.
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.
50 Years of Dilution Refrigeration
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.
ILIAS WG1 - April 7 th, 2005 G.W. ANTENNA NAUTILUS LNF - FRASCATI G.W. ANTENNA EXPLORER CERN - GENEVA Bar Al 5056 M = 2270 kg L = 2.97 m Ø = 0.6 m A =
111 Kazuhiro Yamamoto Institute for Cosmic Ray Research, the University of Tokyo Cryogenic interferometer technologies 19 May 2014 Gravitational Wave Advanced.
LIGO-G Z Silicon as a low thermal noise test mass material S. Rowan, R. Route, M.M. Fejer, R.L. Byer Stanford University P. Sneddon, D. Crooks,
1 Kazuhiro Yamamoto Institute for Cosmic Ray Research The University of Tokyo KAGRA external review (Cryogenic payload) 18 April 2012.
ROG MAT Group: Bassan M., Minenkov Yu., Rocchi A., Simonetti R. – Roma2, INFN Fafone V., Quintieri L. – LNF ILIAS – GW Meeting report May 2004.
1 Kazuhiro Yamamoto Institute for Cosmic Ray Research The university of Tokyo LCGT internal review (Cryogenic payload) 30 January 2012.
1 The control of the Virgo mirrors is realized using coil-magnet actuators Can this technique be used in ET, from room to cryogenic temperatures? Is the.
1 Kazuhiro Yamamoto Institute for Cosmic Ray Research The university of Tokyo LCGT internal review (Cryogenic payload) 30 January 2012.
Active Vibration Isolation using a Suspension Point Interferometer Youichi Aso Dept. Physics, University of Tokyo ASPEN Winter Conference on Gravitational.
E. Majorana (INFN – Rome) ELiTES 3 rd General Meeting Hongo Campus – Tokyo – 9-10 Feb., 2015 Cryogenic platform with vertical suspension: a practical approach.
Lessons from CLIO Masatake Ohashi (ICRR, The University of TOKYO) and CLIO collaborators GWADW2012 Hawaii 2012/5/16.
Yoichi Aso Columbia University, New York, NY, USA University of Tokyo, Tokyo, Japan July 14th th Edoardo Amaldi Conference on Gravitational Waves.
Studying the use of masses on the microwaves cables to isolate seismic noise in the Schenberg Detector. Carlos Frajuca Fábio da Silva Bortoli São Paulo.
Progress Towards a Cryogenic LIGO mirror
Overview of the 20K configuration
New suspension study for LCGT
Cryogenic Test Masses for LIGO Upgrades
MiniGRAIL “Extreme Make-over” Giorgio Frossati
External forces from heat links in cryogenic suspensions
Superattenuator for LF and HF interferometers
Cryogenic Payload Modeling: Vibration via Heat Links
Flat-Top Beam Profile Cavity Prototype: design and preliminary tests
New suspension study for LCGT
Flat-Top Beam Profile Cavity Prototype
Cryogenic Payload Modeling: Vibration via Heat Links
Presentation transcript:

Participants: C-1:Cryogenic last-stage suspensions (interferometers) (F.Ricci-G.Frossati) Objectives: -Design new suspension elements for the last stage of interferometers. -Achieve a low noise remote control of the mirror position using cryogenic sensors -Assemble and test of a full-scale prototype of cryogenic final stage C-2:Cryogenics suspensions for advanced interferometers (G.Frossati- M.Bassan)- Objectives: -Two 1.2 ton spheres with their suspension assembled and measurements of Q and thermal noise at low temperature performed. C-3: Cryogenics suspension system for interferometers (S.Braccini- M.Bassan) Objectives: -The entire apparatus be located in a cryogenic environment; the extra noise coming from the cryogenic system be studied and made negligible. -Full cryogenic suspension be assembled and tested

Participants: Participants: INFN ROG Leiden University Tasks: - Cool down of Minigrail to 50 mK - Investigation of heat transfer from the mixing chamber to the sphere Deliverables:- Report on mechanical transfer function measurements of cryogenic suspension Cryogenic suspension system for advanced resonant detectors

MiniGRAIL Cryogenics cryostat Liquid N 2 77K (-196 ºC) Liquid He 4K (-269 ºC) Dilution refrigerator (10 mK)

MiniGRAIL Cryogenics; The dilution refrigerator still (700 mK) 50 mK plate mixing chamber (10 mK)

To 50 mK shield To mixing chamber Cryogenics Thermal anchoring suspension To still shield

Cryogenics Run 4 Minimum temperatures: T sphere = 80 mK T mc = 20 mK Time dependent heat leak from sphere: 45  W after 6 weeks

Vibration Isolation System Attenuation cables + absorbers

Vibration Isolation System Attenuation between mass 1 and 2

Larger diameter (68 cm instead of 65 cm) gives lower frequency and higher mass (1300 kg instead of 1150 kg). Six holes machined in TIGA positions The new sphere

Resonance frequencies of bare sphere at 300 K Old sphere New sphere Frequency of new sphere about 200 Hz lower

Improvements on the Vibration Isolation System 370 Material  before (mm) f before (Hz) CuAl 1, CuAl 3, Cu

Improvements on the Vibration Isolation System Material  before (mm) f before (Hz)  after (mm) f after (Hz) CuAl 1, CuAl 3, Cu

Improvements on the Vibration Isolation System ~ 50 dB

Closed Membrane Capacitive Transducer Advantages: Compact design Easy to make electrode membrane mass (~ 200 g) spring CuAl6% d ~ 30 micro m V BIAS up to 500 V

Cryogenic run transformer + 2-stage SQUID calibrator

3 hour 5K of mode 3 (2943 Hz) exponential fit T eff = 70 mK

MiniGRAIL sensitivity - run x

MiniGRAIL sensitivity - run 6 Run 6 T5 K  700 ħ Q10 5 M200 g C1.1 nF V bias 200 V Run 7 T80 mK  100 ħ Q10 6 M400 g C1.5 nF V bias 400 V T eff = 40  K 4 x

MiniGRAIL sensitivity - comparison Initial target large interferometers LIGO S3 GEO AURIGA NAUTILUS/EXPLORER MiniGRAIL run 6 Planned at the end of 2004 MiniGRAIL run 7