GEO600 Detector Status Harald Lück Max-Planck Institut für Gravitationsphysik Institut für Atom- und Molekülphysik, Uni Hannover.

Slides:



Advertisements
Similar presentations
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) HOMODYNE AND HETERODYNE READOUT OF A SIGNAL- RECYCLED GRAVITATIONAL WAVE DETECTOR.
Advertisements

19. October 2004 A. Freise Automatic Alignment using the Anderson Technique A. Freise European Gravitational Observatory Roma
The GEO 600 Detector Andreas Freise and the GEO 600 Team University of Hannover May 20, 2002.
Dual Recycling for GEO 600 Andreas Freise, Hartmut Grote Institut für Atom- und Molekülphysik Universität Hannover Max-Planck-Institut für Gravitationsphysik.
Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
T1 task- update Mike Plissi. 2 Collaboration Groups actively involved INFN-VIRGO MAT IGR-Glasgow Groups that have expressed interest INFN-AURIGA CNRS-LKB.
Cascina, January 25th, Coupling of the IMC length noise into the recombined ITF output Raffaele Flaminio EGO and CNRS/IN2P3 Summary - Recombined.
G v1Advanced LIGO1 Status of Ground-Based Gravitational-wave Interferometers July 11, 2012 Daniel Sigg LIGO Hanford Observatory Astrod 5, Bangalore,
Cascina, January 24, 2005 Status of GEO600 Joshua Smith for the GEO600 team.
Optics of GW detectors Jo van den Brand
Status of the LIGO Project
2/9/2006Welcome to LIGO1 Welcome to LIGO!. 2/9/2006Welcome to LIGO2 LIGO: A detector that measures very tiny displacements How tiny?
rd ILIAS-GW annual general meeting 1 VIRGO Commissioning progress J. Marque (EGO)
Q09/2001 The GEO 600 Laser System LIGO-G Z V. Quetschke°, M. Kirchner°, I.Zawischa*, M. Brendel*, C. Fallnich*, S. Nagano +, B. Willke° +, K.
Towards dual recycling with the aid of time and frequency domain simulations M. Malec for the GEO 600 team Max-Planck-Institut für Gravitationsphysik Albert-Einstein-Institut.
GEO600 Harald Lück Ruthe, Worldwide Interferometer Network.
Katrin Dahl for the AEI 10 m Prototype team March 2010 – DPG Hannover Q29.1 Stabilising the distance of 10 m separated.
Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut) Institut für Atom- und Molekülphysik Detector Characterization of GEO 600 during.
Joshua Smith December 2003 Detector Characterization of Dual-Recycled GEO600 Joshua Smith for the GEO600 team.
Design of Stable Power-Recycling Cavities University of Florida 10/05/2005 Volker Quetschke, Guido Mueller.
The GEO 600 Detector Andreas Freise for the GEO 600 Team Max-Planck-Institute for Gravitational Physics University of Hannover May 20, 2002.
Optical readout for a resonant gw bar. Old setup.
Experiments towards beating quantum limits Stefan Goßler for the experimental team of The ANU Centre of Gravitational Physics.
Test mass dynamics with optical springs proposed experiments at Gingin Chunnong Zhao (University of Western Australia) Thanks to ACIGA members Stefan Danilishin.
Interferometer Control Matt Evans …talk mostly taken from…
Experimental Characterization of Frequency Dependent Squeezed Light R. Schnabel, S. Chelkowski, H. Vahlbruch, B. Hage, A. Franzen, N. Lastzka, and K. Danzmann.
GEO‘s experience with Signal Recycling Harald Lück Perugia,
07. July 2004 Andreas Freise Status of VIRGO A. Freise For the Virgo Collaboration European Gravitational Observatory.
T1 task- update Mike Plissi. 2 Motivation  Thermo-elastic noise is higher than the ‘intrinsic’ noise in crystalline materials  There are several sources.
04. November 2004 A. Freise A. Freise, M. Loupias Collaboration Meeting November 04, 2004 Alignment Status.
LISA October 3, 2005 LISA Laser Interferometer Space Antenna Gravitational Physics Program Technical implications Jo van.
Electrostatic actuators: from the GEO experience to the 2 nd generation requirements Harald Lück Perugia,
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.
Variable reflectivity signal-recycling mirror and control Stefan Goßler for the experimental team of The ANU Centre of Gravitational Physics.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v2.
Harald Lückfor the GEO600 Comissioning team 1ILIAS Meeting, Palma, Oct Title GEO 600 Commissioning Status Based on a talk of Stefan Hild for the.
Status of GEO600 Benno Willke for the GEO600 team Aspen Meeting Aspen CO, January 2005 LIGO-G Z.
GEO600 Status Update Harald Lück Hannover, April 2005.
Status of the Advanced LIGO PSL development LSC Virgo meeting, Caltech, March 2008 LIGO G Z Benno Willke for the PSL team.
Abstract The Hannover Thermal Noise Experiment V. Leonhardt, L. Ribichini, H. Lück and K. Danzmann Max-Planck- Institut für Gravitationsphysik We measure.
AIGO 2K Australia - Italy Workshop th October th October 2005 Pablo Barriga for AIGO group.
Perugia, Italy Reducing the Noise in GEO600 Joshua Smith for the GEO 600 team.
ILIAS WG1 meeting Han/Ruthe Harald Lück ILIAS WG1 meeting, Sep. 2004, Hannover/Ruthe GEO Status (Update)
Dual Recycling in GEO 600 H. Grote, A. Freise, M. Malec for the GEO600 team Institut für Atom- und Molekülphysik University of Hannover Max-Planck-Institut.
The status of VIRGO Edwige Tournefier (LAPP-Annecy ) for the VIRGO Collaboration HEP2005, 21st- 27th July 2005 The VIRGO experiment and detection of.
Institute for Cosmic Ray Research Univ. of Tokyo Development of an RSE Interferometer Using the Third Harmonic Demodulation LIGO-G Z Osamu Miyakawa,
ACIGA High Optical Power Test Facility
Initial and Advanced LIGO Status Gregory Harry LIGO/MIT March 24, 2006 March 24, th Eastern Gravity Meeting G R.
Caltech, February 12th1 Virgo central interferometer: commissioning and engineering runs Matteo Barsuglia Laboratoire de l’Accelerateur Lineaire, Orsay.
Ultra-stable, high-power laser systems Patrick Kwee on behalf of AEI Hannover and LZH Advanced detectors session, 26. March 2011 Albert-Einstein-Institut.
Status of GEO600 Benno Willke for the GEO600 team ESF Exploratory Workshop Perugia, September 2005.
ALIGO 0.45 Gpc 2014 iLIGO 35 Mpc 2007 Future Range to Neutron Star Coalescence Better Seismic Isolation Increased Laser Power and Signal Recycling Reduced.
The VIRGO detection system
GEO Status and Prospects Harald Lück ILIAS / ETmeeting Cascina November 2008.
Stefan Hild 1GWADW, Elba, May 2006 Experience with Signal- Recycling in GEO 600 Stefan Hild, AEI Hannover for the GEO-team.
The Proposed Holographic Noise Experiment Rainer Weiss, MIT On behalf of the proposing group Fermi Lab Proposal Review November 3, 2009.
Daniel Sigg, Commissioning Meeting, 11/11/16
The Proposed Holographic Noise Experiment
GEO600 Control aspects where do the error signal come from?
Interferometric speed meter as a low-frequency gravitational-wave detector Helge Müller-Ebhardt Max-Planck-Institut für Gravitationsphysik (AEI) and Leibniz.
Update on the Advanced LIGO PSL Program
Thermal Compensation of the Radius of Curvature of GEO600 Mirrors
Design of Stable Power-Recycling Cavities
Workshop on Gravitational Wave Detectors, IEEE, Rome, October 21, 2004
GEO HF Limits/Goals/Options…
Summary of iKAGRA Test Run Mar 25-31, 2016
LIGO Interferometry CLEO/QELS Joint Symposium on Gravitational Wave Detection, Baltimore, May 24, 2005 Daniel Sigg.
Talk prepared by Stefan Hild AEI Hannover for the GEO-team
Homodyne detection: understanding the laser noise amplitude transfer function Jérôme Degallaix Ilias meeting – June 2007.
Presentation transcript:

GEO600 Detector Status Harald Lück Max-Planck Institut für Gravitationsphysik Institut für Atom- und Molekülphysik, Uni Hannover

Worldwide Interferometer Network

Laser Optical Layout Michelson Interferometer Output Mode Cleaner Mode Cleaners 600m 10 W 5 W 1 W ~ 5 kW 10 kW at Beam Splitter ~50mW Light power (specs)

GEO 600 Sensitivity specs.

Laser Light Power (current) Michelson Interferometer Output Mode Cleaner Mode Cleaners 10W 1W 300W at Beam Splitter 2W2W ~10mW Mode Cleaners: Troughput 80% 72% Finesse Visibility 96% 92% 98.65% Power Recycling Cavity: Mode matching97% Finesse 450 Linewidth 270 Hz

Optical Layout Main Interferometer Mode Cleaner Laser Bench Output Bench

Slave Master Slave entrance to vacuum system Laser System Master Laser: Nd:YAG NPRO (non-planar ring oscillator) 1064 nm Slave Laser: Nd:YAG injection-locked ring cavity nm less than 5% in higher modes Additional Information: Talk: Wednesday 12:40 – 13:10 h Benno Willke Poster session: Tuesday 20:30 – 22:00 h

GEO Triple Pendulum Suspension

Thermal Noise Issues  Monolithic Suspension Silicate (Hydroxy- Catalysis) Bonding Weld

Length and Frequency Control Michelson Interferometer Output Mode Cleaner Laser Mode Cleaners 25 MHz 13 MHz 37 MHz Laser Frequency Stabilisation: no rigid reference cavity laser is directly stabilised to suspended cavities 3 sequential Pound- Drever-Hall control loops common mode of the Power-Recycled Michelson serves as frequency reference

Mode Cleaners Output Mode Cleaner Michelson Length Control Michelson Interferometer Laser 15 MHz 10 MHz Differential arm length: (gravitational wave signal) heterodyne detection Schnupp modulation Signal-Recycling control: separate modulation frequency reflected beam from beam splitter AR coating

Reaction Pendulum: 3 coil-magnet actuators at intermediate mass Electrostatic actuation on test mass bias 500V, range 0-800V=4µm Test Mass Actuators <10Hz >10Hz

Alignment Control differential wave-front sensing spot position control 4 degrees of freedom at MC 1 +4 at MC 2 +4 at MI (common mode) +2 at MI (differential mode) +2 at Signal-Recycling cavity = 36 Alignment Control

Magnet/coil actuators on IM UGF: ~10Hz Diff. MI Fast Auto-Alignment Output port  Reduces misalignment below 50 nrad rms  Reliable locking over long timescales. Duty cycle >95%

Output mode Radii Of Curvature of folding mirrors do not match East ROC: 687m North ROC: 666m Spec: 640m

Thermal adjustment of ROC + -

Thermal adjustment of ROC (II)

15 W 10 W

15 W 20 W

15 W 30 W

15 W 40 W

15 W 50 W

15 W 50 W

15 W 60 W

15 W 70 W

Signal Recycling Mirror Reflectivity = 99% Coil/magnet actuation directly to mirror Triple pendulum suspension with reaction pendulum chain Tunable between 550Hz and 5kHz Mode-healing 2x

Signal Recycling Mirror Reflectivity = 99% Coil/magnet actuation directly to mirror Triple pendulum suspension with reaction pendulum chain Tunable between 550Hz and 5kHz Mode-healing 5 kHz3 kHz 1 kHz

Sensitivity Development Dec Aug Nov Jan % 98.5% 95.2% 98.7%