VIRGO. The status of VIRGO. & INFN - Sezione di Roma 1. 1 / 6/ 2004 Fulvio Ricci

Size: px
Start display at page:

Download "VIRGO. The status of VIRGO. & INFN - Sezione di Roma 1. 1 / 6/ 2004 Fulvio Ricci"

Transcription

1 The status of VIRGO Fulvio Ricci Dipartimento di Fisica - Università di Roma La Sapienza & INFN - Sezione di Roma 1

2 The geometrical effect of Gravitational Waves The signal the metric tensor perturbation h ~ DL / L Interferometric Detection of Gravitational Waves Df = (2p/l)DL ~ h (L/l)

3 DL ~ L * h The interferometer signal DF is proportional to DL so that the arm length L can play the role of amplification factor of the Gravitational signal h L To increase the optical path, the light is trapped inside the arms before the recombination. The Virgo choice is to trap the light by constructing one Fabry Perot cavity for each arm F = h o (wl/c) (2F/p)/ [1+(p W t) 2 ] 1/2 F = Fabry Perot finesse t = cavity storage time L Beam splitter Photo detector

4 Shot Noise Reduction:the Power recycling Power recycling mirror L L S hh 1 / 2 = 1 8LF 4 lc h ( PhR c ) 1 + ( f / f t ) 2 Beam splitter Photo detector F=finesse of the Fabry Perot, h =photodiode efficiency, R c = recycling factor, f t = cut off frequency. R c e f t are functions of the recycling mirror reflectivity Virgo parameters: R c = 50, f t ~500 Hz, incident power on the beam splitter 1 kw

5 The main goals of the CITF Validate most of the Virgo technical choices Input Mode Cleaner Length = 144 m West mirror Suspension performance Locking procedure Alignment and local control performances Laser injection performance Detection strategy test Environmental noise Laser Nd:YAG P=10 W Recycling 6 m 5.6 m 6.4 m North mirror Output Mode Cleaner Length = 4 cm

6 Seismic attenuation direct measurement We measured the attenuation factor of the ground seismic noise and we compared the seismic noise attenuation at the level of the mirror to the thermal pendulum noise Pisa region seismic noise: ~ 10-7 f -2 m/(hz) 1/2 for f < 20 Hz (horizontal & vertical) Thermal pendulum noise: ~ f -5/2 m/(hz) 1/2 The attenuation factor must be smaller than 10-7 f -1/2 Monochromatic excitation injected at the top stage level (vertical and horizontal): if we do not detected any thing at the mirror level, we derive the upper limits. lines Attenuation factor Mirror seismic displacement ( Horizontal) m/(hz) 1/2 Mirror thermal displacement m/(hz) 1/ Hz Hz < < lines 2.25 Hz 4.1 Hz Attenuation factor < 10-8 Mirror seismic displacement ( Vertical) m/(hz) 1/ < Mirror thermal displacement m/(hz) 1/

7 Alignment noise Electronic photodiode noise 09/01 / E0 12/01 / E1 04/02 / E2 05/02 / E3 Frequency laser noise 07/02 / E4 4 orders of magnitude to gain Payload resonances Expected Virgo The CITF lesson: upgrade of the local control Improve the Laser frequency stabilization (investigation/reducti on of the prestabilized laser frequency noise also) Global control upgrade Æ Automatic alignment

8

9 The Active Control of Virgo ITF to be operated as a resonant null instrument FP cavities locked L N, L W Recycling cavity locked l r + (l n +l w )/2 Output on the dark fringe (l n - l w ) The GW signal is extracted from the feedback signal Stringent requirement for locking: r.m.s. mirror motion not to exceed m Since the mirror residual motion (normal modes of the suspension, Earth crust tidal and thermal strain) ~10-3 m The required dynamic range of the control system: >10 9 Can t t be done in a single step

10 Hierarchical Control Use of local sensors to damp the suspension resonances Use the ITF output as a correction signal: split it in bands, use actuators hierarchically IP: 1 mm Ø 1 mm Marionette: 1 mm Ø 1 nm Mirror: 1 nm Ø m

11 The local control: the coarse system It covers the full range provided by mechanical clearence of suspension The position of the mirror respect to the ground is monitored by the using CCD cameras located outside the mirror vacuum chambers In the CITF case the mirror holders are equipped with 4 fiducial points set on the border. Input data are - the mutual distance among the fiducial points - optical system characteristics -sensor - mirror distance

12 Two fine methods An auxiliary laser beam is reflected by the mirror, thane folded by an external auxiliary mirror onto the mirror holder. The spot of the diffused light is monitored by the camera. Once the mirror moves along the direction perpendicular to its reflecting surface

13 Main motivation for upgrading: the recycled interferometer sensitivity was limited by the angular control noise between 1 and 10 Hz. Upgrade targets 1) Damping of pendulum z-oscillation (0.6 Hz) in the CITF it was limited by sensor noise ultimate limit Ë seismic noise (10-7 /f 2 m/hz 1/2 ) 2) Angular control q x and q y : a) Lower noise ( 2 order of magnitudes) b) larger bandwidth BW~2 Hz

14 VIRGO - 3 optical levers, 1 field imaging system - 3 PSD sensors, 1 CCD camera

15 Ê ˆ Á 1- D = Á f Á - 1 Ë f VIRGO The basic equations of the second fine control Virgo mirror lens PSD sensor Ê L 1- D ˆ ˆ Á + D Ë f Ê 1- L x ˆ 1 Á Ë q 1 f Ê x 2 Ê Á x Ë q 2 = 1- D ˆ 2 Á Ë f x + Ê L Ê 1- D ˆ ˆ Á Á 1 Ë f + D q Ë 1 x D x 2 = 1-2 Ê = L 1- D ˆ Á + D x1 f q 1 Ë f In the focal plane of the lens D=f we have x 2 x = 0 2 = f We are not sensitive to translation x1 q 1 In the image plane of the lens D 0 = LF/(L-f) x D x 2 2 = - = 0 x L q 1 1 L D We are not sensitive to the beam rotation ( VIRGO mirror rotation)

16 Sensitivity in the table-top experiment in the image plane Ë Dx 2 = -2(D/L) Dz = Dz in the focal plane Ë Dx 2 = 2 f Da = 0.4 Da Then, (f 0.6 Hz) 10 m / Hz X ~ -7 Ï = ª 2 = Ì -8 Ó (f = 10 Hz) ª 10 m / Hz X ~ Z ~ 7 (0.6 Hz) = 2 ª m / Hz 0.36 ~ X ~ 2 - a (10 Hz) = ª rad / Hz 0.4

17 Residual angular noise - BS payload V/(Hz) 1/2 V/(Hz) 1/2 Q y Frequency (Hz) Q x Frequency (Hz) ~ rad/(hz) 1/2 V Q y V Q x time time

18 The commissioning of VIRGO

19 Phase A: Fabry-Perot cavities Commissioning of interferometer arms Test all aspects of control systems in a simple optical configuration - locking - automatic alignment - second stage of laser frequency stabilization - suspension hierarchical control Verify the performances of the various sub-systems: - injection, detection, global control, DAQ, data storage, - make the list of problems to be solved in a following phase (do no stuck on a problem, if possible!) Phase A1: Commissioning of north arm Verify functioning of NI and NE suspension controls Phase A2: Commissioning of west arm Verify functioning of WI, WE and part of BS suspension controls

20 Phase B: Recombined Interferometer Commissioning of interferometer in recombined mode Useful intermediate step towards full interferometer lock Start noise investigations fi make the list of problems to be solved in a following phase Phase B1: Lock Michelson interferometer Verify functioning of BS longitudinal control Phase B2: Operate Fabry-Perot Michelson interferometer Verify understanding of lock acquisition and linear alignment Start noise investigations (hopefully others than laser noises)

21 Phase C: Recycled Interferometer Commissioning of Recycled Fabry-Perot interferometer Test full locking acquisition process Implement complete wave-front sensing control Noise hunting Phase C1: Lock central interferometer First step of lock acquisition Verify PR mirror longitudinal control Check recycling gain Phase C2: Lock & Operate full interferometer

22 Status of commissioning today Done: Phase A & Phase B - Commissioning of interferometer arms lock of the North arm lock of the West arm - Improve the Laser frequency stabilization (control loop instability) - Investigation/Reduction of the pre-stabilized laser frequency noise - Global control upgrade Æ Automatic alignment - ITF recombination To be done: Phase C - Recycled configuration

23 The Commissioning Runs of Virgo Engineering Runs Central Interferometer E0 (September 21-24, 2001): Simple Michelson configuration illuminated with the auxiliary laser. E1 (December 7-10, 2001): E1 + use of hierarchical suspension control. E2 (April 5-8, 2002): Recycled Michelson configuration illuminated with the auxiliary laser. E3 (May, 16-19, 2002): E2 + use automatic alignment. E4 (July 12-15, 2003): Recycled Michelson illuminated with the Virgo injection system. Virgo A&I runs E4.1 "Silent run" (June 5-6, 2003): Interferometer sub-systems test C0 (July 30-31, 2003): North arm controlled (Inertial Damping and Local Control active) illuminated with a "dirty beam". Virgo Commissioning runs C1 (November 14-17, 2003): North arm Fabry-Perot C2 (February 20-23, 2004): North arm Fabry-Perot with automatic alignment (hopefully) + West arm Fabry-Perot C3 (April 23-27, 2004): North cavity locked with Second Stage Frequency Stabilization and Automatic Alignment

24 Frequency noise reduction

25 The VIRGO optical layout and the injection bench

26 E4 and C1 data analysis Laser frequency noise due to IMC length noise: - Automatic alignment feedback noise - Reference cavity feedback noise Laser frequency noise reduction W/(Hz) 1/2 C1 New IMC control (Feb 5)

27 Laser frequency stabilization Summary of the progress Loop instability problem solved Several important steps accomplished 1) Close second stage of frequency stabilization (SSFS) using the signal provided by B1p (March 23 rd ) 2) Lock north arm to reference cavity signal ( double loop ) (April 8 th ) 3) Use B1 signal (more sensitive) instead of B1p (April 23 rd ) B1p Æ B1

28 C3 run (V) Present laser frequency noise: with and without double loop Hz/(Hz) Hz/sqrt(Hz) 1/2 without double loop with double loop Frequency [Hz]

29 Laser frequency noise - C3 run Present laser frequency noise: effect in Virgo Hypothesis: - C3 error signal spectrum = laser frequency noise spectrum - recycling cavity low-pass will be at 10 Hz - common mode rejection factor /sqrt(Hz)

30 Angular control and automatic Alignment

31 Automatic alignment Global control upgraded to include the control loops for the alignment of the North arm at the end of January Linear alignment ON Linear alignment OFF

32 C2 run (I) Two different configurations tested 1) North arm locked to B1 (OMC also locked) + automatic alignment of NI and NE 2) West arm locked to B1 (OMC also locked) February 20-23

33 Earth Tidal Compensation

34 Earth Tidal prediction A computer program called ETGTAB has been adapted to the Virgo configuration. The magnitude of the elongation of the three km arms is of the order of 200 mm peak to peak. The magnitude of the tower tilts is of the order of 100 nrad. During the C3 run several delocks of the North cavity were observed due to the limited dynamic range of the z correction of the reference mass coil. The data points have been adjusted by an offset: for each set we have a scale factor of 10 microns per volt and a phase offset of 40 minutes in time. The agreement is good indicating that we can predict and compensate for the earth tides.

35 Earth Tidal Compensation Suspension Point Control The Filter 7 monitoring was also used as a basis for the diagonalization of the driving of the suspension top stage along the VIRGO Global Reference System (VGRS). The chain suspension point can be moved independently along z, x, q y, using the three top stage coil-magnet actuators. Tidal Control: Thanks to the diagonalization, changing the z-offset of the Inertial Damping loops expressed in VGRS, a pure displacement of the top stage along the beam direction can be achieved. Since in the low frequency range the mirror and the top-stage move coherently, this is used for the tidal control from the top-stage. The low frequency part of the error signal of the interferometer along the beam is sent to the top stage offset along z in VGRS.

36 Phase A: Single Arm sensitivity and noise study

37 C2 sensitivity MC length noise Sensitive to scroll pumps MC length control noise ADC noise Shot noise

38 C3 compared to C2 Input Bench resonances Above 150 Hz : Below 100 Hz : laser frequency noise has been reduced but IB resonances are still visible the same noise structures still exist

39 Sensitivities for the single arm configuration m/sqrt(hz) C2 C1 C3

40 Phase B: the recombined Interferometer Noise study and sensitivity

41 Michelson Fabry-Perot in the arms VIRGO Phase B (recombined ITF): power loss B8 600 mw T=50 ppm When the recycling mirror is misaligned, the transmitted beam is just the 8% of the total incident power. 3 dof (2 coupled) 10 W T=8% 0.8 W T=12% T=12% The light on photodiodes is weak: SNR ~ 500 times lower of that of the final VIRGO configuration 600 mw B7 B5 200 mw R= T=50 ppm B2 64 mw B1p 8 mw (white fringe)

42 Summary : Noise sources for recombined Laser frequency noise B8 electronic noise electronic/shot noise??

43 Sensitivity of the recombined configuration with new filter C3 recombined sensitivity sensitivity with new filter Above 300 Hz : B8_ACp not used any more fi noise has decreased New structures to be understood

44 Conclusion 1 - North arm High frequencies : Electronic noise lower than shot noise but sensitivity now limited by a noise coming from the ITF > 250 Hz : not understood (frequency noise?) fi to be investigated Between 10 & 250 Hz : coherence with the correction signals used by the IMC Automatic Alignment loop fi probably injects Input Bench resonances 2 - Recombined configuration High frequencies : unknown noise adding to the photodiodes electronic noise Hz : B8 electronic noise Hz : laser frequency noise

45 1/sqrt(Hz) Frequency (Hz)

46 Several important results obtained in this year - Fabry-Perot automatic alignment - Laser frequency stabilization - Lock of the recombined interferometer VIRGO Conclusions Several problems found and solved or being addressed - Diaphragm - Aberrations - Anderson offset - Local control lasers - and a lot of small bugs Several problems found and to be solved - Input bench resonances - Dihedron displacements - Power recycling mirror resonances - Diffused light inside the input mode-cleaner - Size of optics on input bench - Spurious beams

47 Mid term plan Complete commissioning of recombined interferometer by June New commissioning run (C4) at the end of June (two months after C3) Start commissioning of recycled interferometer in June - Re-run PR-NI - Run CITF - First full-locking trials during the summer New run (C5) at the end of the summer

Virgo status and commissioning results

Virgo status and commissioning results Virgo status and commissioning results L. Di Fiore for the Virgo Collaboration 5th LISA Symposium 13 july 2004 VIRGO is an French-Italian collaboration for Gravitational Wave research with a 3 km long

More information

The VIRGO detection system

The VIRGO detection system LIGO-G050017-00-R Paolo La Penna European Gravitational Observatory INPUT R =35 R=0.9 curv =35 0m 95 MOD CLEAN ER (14m )) WI N d:yag plar=0 ne.8 =1λ 064nm 3km 20W 6m 66.4m M odulat or PR BS N I sing lefrequ

More information

Advanced Virgo commissioning challenges. Julia Casanueva on behalf of the Virgo collaboration

Advanced Virgo commissioning challenges. Julia Casanueva on behalf of the Virgo collaboration Advanced Virgo commissioning challenges Julia Casanueva on behalf of the Virgo collaboration GW detectors network Effect on Earth of the passage of a GW change on the distance between test masses Differential

More information

The Virgo detector. L. Rolland LAPP-Annecy GraSPA summer school L. Rolland GraSPA2013 Annecy le Vieux

The Virgo detector. L. Rolland LAPP-Annecy GraSPA summer school L. Rolland GraSPA2013 Annecy le Vieux The Virgo detector The Virgo detector L. Rolland LAPP-Annecy GraSPA summer school 2013 1 Table of contents Principles Effect of GW on free fall masses Basic detection principle overview Are the Virgo mirrors

More information

Commissioning of Advanced Virgo

Commissioning of Advanced Virgo Commissioning of Advanced Virgo VSR1 VSR4 VSR5/6/7? Bas Swinkels, European Gravitational Observatory on behalf of the Virgo Collaboration GWADW Takayama, 26/05/2014 B. Swinkels Adv. Virgo Commissioning

More information

The VIRGO injection system

The VIRGO injection system INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1829 1833 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)29349-1 The VIRGO injection system F Bondu, A Brillet, F Cleva, H Heitmann, M Loupias,

More information

Interferometer signal detection system for the VIRGO experiment. VIRGO collaboration

Interferometer signal detection system for the VIRGO experiment. VIRGO collaboration Interferometer signal detection system for the VIRGO experiment VIRGO collaboration presented by Raffaele Flaminio L.A.P.P., Chemin de Bellevue, Annecy-le-Vieux F-74941, France Abstract VIRGO is a laser

More information

Installation and Characterization of the Advanced LIGO 200 Watt PSL

Installation and Characterization of the Advanced LIGO 200 Watt PSL Installation and Characterization of the Advanced LIGO 200 Watt PSL Nicholas Langellier Mentor: Benno Willke Background and Motivation Albert Einstein's published his General Theory of Relativity in 1916,

More information

The VIRGO suspensions

The VIRGO suspensions INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1623 1629 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)30082-0 The VIRGO suspensions The VIRGO Collaboration (presented by S Braccini) INFN,

More information

Advanced Virgo Technical Design Report

Advanced Virgo Technical Design Report Advanced Virgo Technical Design Report VIR xxxa 12 Issue 1 The Virgo Collaboration March 21, 2012 Contents 1 ISC 1 1.1 General description of the sub-system........................ 1 1.2 Input from other

More information

Superattenuator seismic isolation measurements by Virgo interferometer: a comparison with the future generation antenna requirements

Superattenuator seismic isolation measurements by Virgo interferometer: a comparison with the future generation antenna requirements European Commission FP7, Grant Agreement 211143 Superattenuator seismic isolation measurements by Virgo interferometer: a comparison with the future generation antenna requirements ET-025-09 S.Braccini

More information

The AEI 10 m Prototype. June Sina Köhlenbeck for the 10m Prototype Team

The AEI 10 m Prototype. June Sina Köhlenbeck for the 10m Prototype Team The AEI 10 m Prototype June 2014 - Sina Köhlenbeck for the 10m Prototype Team The 10m Prototype Seismic attenuation system Suspension Platform Inteferometer SQL Interferometer Suspensions 2 The AEI 10

More information

How to Build a Gravitational Wave Detector. Sean Leavey

How to Build a Gravitational Wave Detector. Sean Leavey How to Build a Gravitational Wave Detector Sean Leavey Supervisors: Dr Stefan Hild and Prof Ken Strain Institute for Gravitational Research, University of Glasgow 6th May 2015 Gravitational Wave Interferometry

More information

7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7)

7th Edoardo Amaldi Conference on Gravitational Waves (Amaldi7) Journal of Physics: Conference Series (8) 4 doi:.88/74-6596///4 Lock Acquisition Studies for Advanced Interferometers O Miyakawa, H Yamamoto LIGO Laboratory 8-34, California Institute of Technology, Pasadena,

More information

A Thermal Compensation System for the gravitational wave detector Virgo

A Thermal Compensation System for the gravitational wave detector Virgo A Thermal Compensation System for the gravitational wave detector Virgo M. Di Paolo Emilio University of L Aquila and INFN Roma Tor Vergata On behalf of the Virgo Collaboration Index: 1) Thermal Lensing

More information

A gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses.

A gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses. A gravitational wave is a differential strain in spacetime. Equivalently, it is a differential tidal force that can be sensed by multiple test masses. Plus-polarization Cross-polarization 2 Any system

More information

Interferometer for LCGT 1st Korea Japan Workshop on Korea University Jan. 13, 2012 Seiji Kawamura (ICRR, Univ. of Tokyo)

Interferometer for LCGT 1st Korea Japan Workshop on Korea University Jan. 13, 2012 Seiji Kawamura (ICRR, Univ. of Tokyo) Interferometer for LCGT 1st Korea Japan Workshop on LCGT @ Korea University Jan. 13, 2012 Seiji Kawamura (ICRR, Univ. of Tokyo) JGW G1200781 v01 Outline Resonant Sideband Extraction interferometer Length

More information

PRM SRM. Grav. Wave ReadOut

PRM SRM. Grav. Wave ReadOut Nov. 6-9,2 The 22nd Advanced ICFA Beam Dynamics Workshop on Ground Motion in Future Accelerators November 6-9, 2 SLAC Passive Ground Motion Attenuation and Inertial Damping in Gravitational Wave Detectors

More information

Angular control of Advanced Virgo suspended benches

Angular control of Advanced Virgo suspended benches Angular control of Advanced Virgo suspended benches Michał Was for the DET and SBE team LAPP/IN2P3 - Annecy Michał Was (LAPP/IN2P3 - Annecy) GWADW, Elba, 2016 May 25 1 / 12 Suspended benches in Advanced

More information

Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech. LIGO-G v1

Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech. LIGO-G v1 Koji Arai / Stan Whitcomb LIGO Laboratory / Caltech LIGO-G1401144-v1 General Relativity Gravity = Spacetime curvature Gravitational wave = Wave of spacetime curvature Gravitational waves Generated by motion

More information

R. De Rosa INFN Napoli For the VIRGO collaboration

R. De Rosa INFN Napoli For the VIRGO collaboration R. De Rosa INFN Napoli For the VIRGO collaboration The lesson of VIRGO+ and VIRGO Science Runs; The Technical Design Report of the Advanced VIRGO project; Conclusion. CSN2 - Frascati, 16-18 Aprile 2012

More information

The generation and application of squeezed light in gravitational wave detectors and status of the POLIS project

The generation and application of squeezed light in gravitational wave detectors and status of the POLIS project The generation and application of squeezed light in gravitational wave detectors and status of the POLIS project De Laurentis* on behalf of POLIS collaboration *Università degli studi di Napoli 'Federico

More information

Control Servo Design for Inverted Pendulum

Control Servo Design for Inverted Pendulum JGW-T1402132-v2 Jan. 14, 2014 Control Servo Design for Inverted Pendulum Takanori Sekiguchi 1. Introduction In order to acquire and keep the lock of the interferometer, RMS displacement or velocity of

More information

DRAFT Expected performance of type-bp SAS in bkagra

DRAFT Expected performance of type-bp SAS in bkagra DRAFT Expected performance of type-bp SAS in bkagra December 27, 216 Yoshinori Fujii Table of Contents 1 Expected performance of type-bp SAS in bkagra 2 1.1 Overview.................................................

More information

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Electrical Engineering and Computer Science

MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Electrical Engineering and Computer Science Student Name Date MASSACHUSETTS INSTITUTE OF TECHNOLOGY Department of Electrical Engineering and Computer Science 6.161 Modern Optics Project Laboratory Laboratory Exercise No. 6 Fall 2010 Solid-State

More information

Improving seismic isolation in Advanced LIGO using a ground rotation sensor

Improving seismic isolation in Advanced LIGO using a ground rotation sensor Improving seismic isolation in Advanced LIGO using a ground rotation sensor 04/16/2016 Krishna Venkateswara for UW- Michael Ross, Charlie Hagedorn, and Jens Gundlach aligo SEI team LIGO-G1600083 1 Contents

More information

Results from the Stanford 10 m Sagnac interferometer

Results from the Stanford 10 m Sagnac interferometer INSTITUTE OF PHYSICSPUBLISHING Class. Quantum Grav. 19 (2002) 1585 1589 CLASSICAL ANDQUANTUM GRAVITY PII: S0264-9381(02)30157-6 Results from the Stanford 10 m Sagnac interferometer Peter T Beyersdorf,

More information

visibility values: 1) V1=0.5 2) V2=0.9 3) V3=0.99 b) In the three cases considered, what are the values of FSR (Free Spectral Range) and

visibility values: 1) V1=0.5 2) V2=0.9 3) V3=0.99 b) In the three cases considered, what are the values of FSR (Free Spectral Range) and EXERCISES OF OPTICAL MEASUREMENTS BY ENRICO RANDONE AND CESARE SVELTO EXERCISE 1 A CW laser radiation (λ=2.1 µm) is delivered to a Fabry-Pérot interferometer made of 2 identical plane and parallel mirrors

More information

Some Progress In The Development Of An Optical Readout System For The LISA Gravitational Reference Sensor

Some Progress In The Development Of An Optical Readout System For The LISA Gravitational Reference Sensor Some Progress In The Development Of An Optical Readout System For The LISA Gravitational Reference Sensor Fausto ~cernese*', Rosario De ~ osa*~, Luciano Di Fiore*, Fabio ~arufi*', Adele La ~ana*' and Leopoldo

More information

Mechanical modeling of the Seismic Attenuation System for AdLIGO

Mechanical modeling of the Seismic Attenuation System for AdLIGO Mechanical modeling of the Seismic Attenuation System for AdLIGO Candidato: Valerio Boschi Relatore interno: Prof. Virginio Sannibale Relatore esterno: Prof. Diego Passuello 1 Introduction LIGO Observatories

More information

EE119 Introduction to Optical Engineering Fall 2009 Final Exam. Name:

EE119 Introduction to Optical Engineering Fall 2009 Final Exam. Name: EE119 Introduction to Optical Engineering Fall 2009 Final Exam Name: SID: CLOSED BOOK. THREE 8 1/2 X 11 SHEETS OF NOTES, AND SCIENTIFIC POCKET CALCULATOR PERMITTED. TIME ALLOTTED: 180 MINUTES Fundamental

More information

arxiv: v1 [gr-qc] 10 Sep 2007

arxiv: v1 [gr-qc] 10 Sep 2007 LIGO P070067 A Z A novel concept for increasing the peak sensitivity of LIGO by detuning the arm cavities arxiv:0709.1488v1 [gr-qc] 10 Sep 2007 1. Introduction S. Hild 1 and A. Freise 2 1 Max-Planck-Institut

More information

Development of the accelerometer for cryogenic experiments II

Development of the accelerometer for cryogenic experiments II Development of the accelerometer for cryogenic experiments II ICRR Univ. of Tokyo, KEK A, Dept. of advanced materials science Univ. of Tokyo B K. Yamamoto, H. Hayakawa, T. Uchiyama, S. Miyoki, H. Ishitsuka,

More information

Optical lever for KAGRA

Optical lever for KAGRA Optical lever for KAGRA Kazuhiro Agatsuma 2014/May/16 2014/May/16 GW monthly seminar at Tokyo 1 Contents Optical lever (OpLev) development for KAGRA What is the optical lever? Review of OpLev in TAMA-SAS

More information

An optical transduction chain for the AURIGA detector

An optical transduction chain for the AURIGA detector An optical transduction chain for the AURIGA detector L. Conti, F. Marin, M. De Rosa, G. A. Prodi, L. Taffarello, J. P. Zendri, M. Cerdonio, S. Vitale Dipartimento di Fisica, Università di Trento, and

More information

5 Advanced Virgo: interferometer configuration

5 Advanced Virgo: interferometer configuration 5 Advanced Virgo: interferometer configuration 5.1 Introduction This section describes the optical parameters and configuration of the AdV interferometer. The optical layout and the main parameters of

More information

Vibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer)

Vibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer) Vibration measurement in the cryogenic interferometric gravitational wave detector (CLIO interferometer) ICRR Univ. of Tokyo, Dept. of geophysics Kyoto University A, KEK B, Dept. of advanced materials

More information

Wavelength Control and Locking with Sub-MHz Precision

Wavelength Control and Locking with Sub-MHz Precision Wavelength Control and Locking with Sub-MHz Precision A PZT actuator on one of the resonator mirrors enables the Verdi output wavelength to be rapidly tuned over a range of several GHz or tightly locked

More information

The Florida control scheme. Guido Mueller, Tom Delker, David Reitze, D. B. Tanner

The Florida control scheme. Guido Mueller, Tom Delker, David Reitze, D. B. Tanner The Florida control scheme Guido Mueller, Tom Delker, David Reitze, D. B. Tanner Department of Physics, University of Florida, Gainesville 32611-8440, Florida, USA The most likely conguration for the second

More information

Arm Cavity Finesse for Advanced LIGO

Arm Cavity Finesse for Advanced LIGO LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T070303-01-D Date: 2007/12/20 Arm Cavity Finesse

More information

TNI mode cleaner/ laser frequency stabilization system

TNI mode cleaner/ laser frequency stabilization system LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T000077-00- R 8/10/00 TNI mode cleaner/ laser frequency

More information

10W Injection-Locked CW Nd:YAG laser

10W Injection-Locked CW Nd:YAG laser 10W Injection-Locked CW Nd:YAG laser David Hosken, Damien Mudge, Peter Veitch, Jesper Munch Department of Physics The University of Adelaide Adelaide SA 5005 Australia Talk Outline Overall motivation ACIGA

More information

ADVANCED VIRGO at the DAWN WORKSHOP

ADVANCED VIRGO at the DAWN WORKSHOP Giovanni Losurdo Advanced Virgo Project Leader for the Virgo Collaboration and EGO ADVANCED VIRGO at the DAWN WORKSHOP DAWN Workshop, May 8, 2015 G Losurdo - AdV Project Leader 1 ADVANCED VIRGO! Participated

More information

Development of Optical lever system of the 40 meter interferometer

Development of Optical lever system of the 40 meter interferometer LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note x/xx/99 LIGO-T99xx- - D Development of Optical lever system

More information

Alessio Rocchi, INFN Tor Vergata

Alessio Rocchi, INFN Tor Vergata Topics in Astroparticle and Underground Physics Torino 7-11 September 2015 Alessio Rocchi, INFN Tor Vergata On behalf of the TCS working group AdVirgo optical layout The best optics that current technology

More information

Alignment control of GEO 600

Alignment control of GEO 600 INSTITUTE OF PHYSICS PUBLISHING Class. Quantum Grav. 1 (4) S441 S449 CLASSICAL AND QUANTUM GRAVITY PII: S64-9381(4)683-1 Alignment of GEO 6 HGrote 1, G Heinzel 1,AFreise 1,SGoßler 1, B Willke 1,HLück 1,

More information

Our 10m Interferometer Prototype

Our 10m Interferometer Prototype Our 10m Interferometer Prototype KAGRA f2f, February 14, 2014 Fumiko Kawaoze AEI 10 m Prototype 1 10m Prototype Interferometer Standard Quantum Limit experiment Macroscopic Quantum mechanics Thermal Noise

More information

Stable Recycling Cavities for Advanced LIGO

Stable Recycling Cavities for Advanced LIGO Stable Recycling Cavities for Advanced LIGO Guido Mueller University of Florida 08/16/2005 Table of Contents Stable vs. unstable recycling cavities Design of stable recycling cavity Design drivers Spot

More information

CHAPTER 3. Multi-stage seismic attenuation system

CHAPTER 3. Multi-stage seismic attenuation system CHAPTER 3 Multi-stage seismic attenuation system With the detection of gravitational waves, mankind has made its most precise distance measurement to date. This would not have been achievable without the

More information

OPTICS IN MOTION. Introduction: Competing Technologies: 1 of 6 3/18/2012 6:27 PM.

OPTICS IN MOTION. Introduction: Competing Technologies:  1 of 6 3/18/2012 6:27 PM. 1 of 6 3/18/2012 6:27 PM OPTICS IN MOTION STANDARD AND CUSTOM FAST STEERING MIRRORS Home Products Contact Tutorial Navigate Our Site 1) Laser Beam Stabilization to design and build a custom 3.5 x 5 inch,

More information

Experience with Signal- Recycling in GEO600

Experience with Signal- Recycling in GEO600 Experience with Signal- Recycling in GEO600 Stefan Hild, AEI Hannover for the GEO-team Stefan Hild 1 GWADW, Elba, May 2006 Stefan Hild 2 GWADW, Elba, May 2006 Motivation GEO600 is the 1st large scale GW

More information

Virgo and the quest for low frequency sensitivity in GW detectors. Adalberto Giazotto INFN Pisa

Virgo and the quest for low frequency sensitivity in GW detectors. Adalberto Giazotto INFN Pisa Virgo and the quest for low frequency sensitivity in GW detectors Adalberto Giazotto INFN Pisa What we found established when we entered in the GW business in 1982 and afterword? 1) Indirect Evidence of

More information

Optical Vernier Technique for Measuring the Lengths of LIGO Fabry-Perot Resonators

Optical Vernier Technique for Measuring the Lengths of LIGO Fabry-Perot Resonators LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY -LIGO- CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Technical Note LIGO-T97074-0- R 0/5/97 Optical Vernier Technique for

More information

TSBB09 Image Sensors 2018-HT2. Image Formation Part 1

TSBB09 Image Sensors 2018-HT2. Image Formation Part 1 TSBB09 Image Sensors 2018-HT2 Image Formation Part 1 Basic physics Electromagnetic radiation consists of electromagnetic waves With energy That propagate through space The waves consist of transversal

More information

GAS (Geometric Anti Spring) filter and LVDT (Linear Variable Differential Transformer) Enzo Tapia Lecture 2. KAGRA Lecture 2 for students

GAS (Geometric Anti Spring) filter and LVDT (Linear Variable Differential Transformer) Enzo Tapia Lecture 2. KAGRA Lecture 2 for students GAS (Geometric Anti Spring) filter and LVDT (Linear Variable Differential Transformer) Enzo Tapia Lecture 2 1 Vibration Isolation Systems GW event induces a relative length change of about 10^-21 ~ 10^-22

More information

DESIGN OF COMPACT PULSED 4 MIRROR LASER WIRE SYSTEM FOR QUICK MEASUREMENT OF ELECTRON BEAM PROFILE

DESIGN OF COMPACT PULSED 4 MIRROR LASER WIRE SYSTEM FOR QUICK MEASUREMENT OF ELECTRON BEAM PROFILE 1 DESIGN OF COMPACT PULSED 4 MIRROR LASER WIRE SYSTEM FOR QUICK MEASUREMENT OF ELECTRON BEAM PROFILE PRESENTED BY- ARPIT RAWANKAR THE GRADUATE UNIVERSITY FOR ADVANCED STUDIES, HAYAMA 2 INDEX 1. Concept

More information

SA210-Series Scanning Fabry Perot Interferometer

SA210-Series Scanning Fabry Perot Interferometer 435 Route 206 P.O. Box 366 PH. 973-579-7227 Newton, NJ 07860-0366 FAX 973-300-3600 www.thorlabs.com technicalsupport@thorlabs.com SA210-Series Scanning Fabry Perot Interferometer DESCRIPTION: The SA210

More information

LIGO II Photon Drive Conceptual Design

LIGO II Photon Drive Conceptual Design LIGO II Photon Drive Conceptual Design LIGO-T000113-00-R M. Zucker 10/13/00 ABSTRACT LIGO II will require very small forces to actuate the final stage test masses, due to the high isolation factor and

More information

Squeezed light and radiation pressure effects in suspended interferometers. Thomas Corbitt

Squeezed light and radiation pressure effects in suspended interferometers. Thomas Corbitt Squeezed light and radiation pressure effects in suspended interferometers Thomas Corbitt MIT Sarah Ackley, Tim Bodiya, Keisuke Goda, David Ottaway, Eugeniy Mihkailov, Daniel Sigg, Nicolas, Smith, Chris

More information

Lasers for Advanced Interferometers

Lasers for Advanced Interferometers Lasers or Advanced Intererometers Benno Willke Aspen Meeting Aspen CO, February 2004 G040041-00-Z Requirements - Topology Sagnac: broadband source to reduce scattered light noise power control recycled

More information

Optical Recombination of the LIGO 40-m Gravitational Wave Interferometer

Optical Recombination of the LIGO 40-m Gravitational Wave Interferometer Optical Recombination of the LIGO 40-m Gravitational Wave Interferometer T.T. Lyons, * A. Kuhnert, F.J. Raab, J.E. Logan, D. Durance, R.E. Spero, S. Whitcomb, B. Kells LIGO Project, California Institute

More information

LIGO-P R Detector Description and Performance for the First Coincidence Observations between LIGO and GEO

LIGO-P R Detector Description and Performance for the First Coincidence Observations between LIGO and GEO LIGO-P030024-00-R Detector Description and Performance for the First Coincidence Observations between LIGO and GEO α??,1, a INFN, Sezione di Pisa, I-56100 Pisa, Italy Abstract For 17 days in August and

More information

The LTP interferometer aboard SMART-2

The LTP interferometer aboard SMART-2 The LTP interferometer aboard SMART-2 Gerhard Heinzel Max-Planck-Institut für Gravitationsphysik, (Albert-Einstein-Institut), Hannover, presented at the LISA Symposium, PSU, 22.7.2002 1 What is SMART-2?

More information

Multiply Resonant EOM for the LIGO 40-meter Interferometer

Multiply Resonant EOM for the LIGO 40-meter Interferometer LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY LIGO-XXXXXXX-XX-X Date: 2009/09/25 Multiply Resonant EOM for the LIGO

More information

Testbed for prototypes of the LISA point-ahead angle mechanism

Testbed for prototypes of the LISA point-ahead angle mechanism Testbed for prototypes of the LISA point-ahead angle mechanism, Benjamin Sheard, Gerhard Heinzel and Karsten Danzmann Albert-Einstein-Institut Hannover 7 th LISA Symposium Barcelona, 06/16/2008 Point-ahead

More information

CHAPTER 5 FINE-TUNING OF AN ECDL WITH AN INTRACAVITY LIQUID CRYSTAL ELEMENT

CHAPTER 5 FINE-TUNING OF AN ECDL WITH AN INTRACAVITY LIQUID CRYSTAL ELEMENT CHAPTER 5 FINE-TUNING OF AN ECDL WITH AN INTRACAVITY LIQUID CRYSTAL ELEMENT In this chapter, the experimental results for fine-tuning of the laser wavelength with an intracavity liquid crystal element

More information

Difrotec Product & Services. Ultra high accuracy interferometry & custom optical solutions

Difrotec Product & Services. Ultra high accuracy interferometry & custom optical solutions Difrotec Product & Services Ultra high accuracy interferometry & custom optical solutions Content 1. Overview 2. Interferometer D7 3. Benefits 4. Measurements 5. Specifications 6. Applications 7. Cases

More information

Model Independent Numerical Procedure for the Diagonalization of a Multiple Input Multiple Output Dynamic System

Model Independent Numerical Procedure for the Diagonalization of a Multiple Input Multiple Output Dynamic System 1588 IEEE TRANSACTIONS ON NUCLEAR SCIENCE, VOL. 58, NO. 4, AUGUST 2011 Model Independent Numerical Procedure for the Diagonalization of a Multiple Input Multiple Output Dynamic System Gianluca Persichetti,

More information

Week IX: INTERFEROMETER EXPERIMENTS

Week IX: INTERFEROMETER EXPERIMENTS Week IX: INTERFEROMETER EXPERIMENTS Notes on Adjusting the Michelson Interference Caution: Do not touch the mirrors or beam splitters they are front surface and difficult to clean without damaging them.

More information

Parametric signal amplification

Parametric signal amplification Parametric signal amplification ET meeting @ Birmingham Mar 27, 2017 K.Somiya Observation of high freq GW sources [Kiuchi, 2010] BNS merger with different models D=100Mpc BNS merger appears above the cavity

More information

LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY

LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Document Type LIGO-T950112-00- D 31 Oct 95 ASC Optical Lever Specification

More information

Thermal correction of the radii of curvature of mirrors for GEO 600

Thermal correction of the radii of curvature of mirrors for GEO 600 INSTITUTE OF PHYSICS PUBLISHING Class. Quantum Grav. 21 (2004) S985 S989 CLASSICAL AND QUANTUM GRAVITY PII: S0264-9381(04)68250-5 Thermal correction of the radii of curvature of mirrors for GEO 600 HLück

More information

PHYS 3153 Methods of Experimental Physics II O2. Applications of Interferometry

PHYS 3153 Methods of Experimental Physics II O2. Applications of Interferometry Purpose PHYS 3153 Methods of Experimental Physics II O2. Applications of Interferometry In this experiment, you will study the principles and applications of interferometry. Equipment and components PASCO

More information

Virgo change request

Virgo change request Virgo change request Quadrants photodiodes for BMS and MC end mirror Responsible: Name: Cleva Email Cleva.at.obs-nice.fr Institution: CNRS / OCA Artemis Procedure start date: 21/12/2006 Procedure end date:

More information

Advanced Virgo phase cameras

Advanced Virgo phase cameras Journal of Physics: Conference Series PAPER OPEN ACCESS Advanced Virgo phase cameras To cite this article: L van der Schaaf et al 2016 J. Phys.: Conf. Ser. 718 072008 View the article online for updates

More information

Quantum States of Light and Giants

Quantum States of Light and Giants Quantum States of Light and Giants MIT Corbitt, Bodiya, Innerhofer, Ottaway, Smith, Wipf Caltech Bork, Heefner, Sigg, Whitcomb AEI Chen, Ebhardt-Mueller, Rehbein QEM-2, December 2006 Ponderomotive predominance

More information

A simple high-sensitivity interferometric position sensor for test mass control on an advanced LIGO interferometer

A simple high-sensitivity interferometric position sensor for test mass control on an advanced LIGO interferometer Optical and Quantum Electronics 31: 571±582, 1999. Ó 1999 Kluwer Academic Publishers. Printed in the Netherlands. 571 A simple high-sensitivity interferometric position sensor for test mass control on

More information

Gingin High Optical Power Test Facility

Gingin High Optical Power Test Facility Institute of Physics Publishing Journal of Physics: Conference Series 32 (2006) 368 373 doi:10.1088/1742-6596/32/1/056 Sixth Edoardo Amaldi Conference on Gravitational Waves Gingin High Optical Power Test

More information

CMS Note Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland

CMS Note Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland Available on CMS information server CMS NOTE 1998/16 The Compact Muon Solenoid Experiment CMS Note Mailing address: CMS CERN, CH-1211 GENEVA 23, Switzerland January 1998 Performance test of the first prototype

More information

PUSHING THE ADVANCED VIRGO INTERFEROMETER TO THE LIMIT

PUSHING THE ADVANCED VIRGO INTERFEROMETER TO THE LIMIT HIGH-PERFORMANCE VIBRATION ISOLATION FOR GRAVITATIONAL WAVE DETECTORS PUSHING THE ADVANCED VIRGO INTERFEROMETER TO THE LIMIT After fifty years of building gravitational wave detectors with everincreasing

More information

CONTROLS CONSIDERATIONS FOR NEXT GENERATION GW DETECTORS

CONTROLS CONSIDERATIONS FOR NEXT GENERATION GW DETECTORS CONTROLS CONSIDERATIONS FOR NEXT GENERATION GW DETECTORS CONTROLS WORKSHOP GWADW 26 MAY 2016 AGENDA Introduction (

More information

Fabry Perot Resonator (CA-1140)

Fabry Perot Resonator (CA-1140) Fabry Perot Resonator (CA-1140) The open frame Fabry Perot kit CA-1140 was designed for demonstration and investigation of characteristics like resonance, free spectral range and finesse of a resonator.

More information

Experimental Test of an Alignment Sensing Scheme for a Gravitational-wave Interferometer

Experimental Test of an Alignment Sensing Scheme for a Gravitational-wave Interferometer Experimental Test of an Alignment Sensing Scheme for a Gravitational-wave Interferometer Nergis Mavalvala *, Daniel Sigg and David Shoemaker LIGO Project Department of Physics and Center for Space Research,

More information

Designing Optical Layouts for AEI s 10 meter Prototype. Stephanie Wiele August 5, 2008

Designing Optical Layouts for AEI s 10 meter Prototype. Stephanie Wiele August 5, 2008 Designing Optical Layouts for AEI s 10 meter Prototype Stephanie Wiele August 5, 2008 This summer I worked at the Albert Einstein Institute for Gravitational Physics as a member of the 10 meter prototype

More information

Stabilizing an Interferometric Delay with PI Control

Stabilizing an Interferometric Delay with PI Control Stabilizing an Interferometric Delay with PI Control Madeleine Bulkow August 31, 2013 Abstract A Mach-Zhender style interferometric delay can be used to separate a pulses by a precise amount of time, act

More information

A Geodetic Reference Frame for the Virgo Interferometer

A Geodetic Reference Frame for the Virgo Interferometer A Geodetic Reference Frame for the Virgo Interferometer A. Paoli - European Gravitational Observatory M. Marsella, C. Nardinocchi - Università di Roma La Sapienza L. Vittuari, A. Zanutta - Università di

More information

1.6 Beam Wander vs. Image Jitter

1.6 Beam Wander vs. Image Jitter 8 Chapter 1 1.6 Beam Wander vs. Image Jitter It is common at this point to look at beam wander and image jitter and ask what differentiates them. Consider a cooperative optical communication system that

More information

Ultra stable high power laser for the VIRGO project

Ultra stable high power laser for the VIRGO project Ultra stable high power laser for the VIRGO project C.N. Man To cite this version: C.N. Man. Ultra stable high power laser for the VIRGO project. International Conference: Laser M2P 3, 1993, Lyon, France.

More information

Adaptive Optics for LIGO

Adaptive Optics for LIGO Adaptive Optics for LIGO Justin Mansell Ginzton Laboratory LIGO-G990022-39-M Motivation Wavefront Sensor Outline Characterization Enhancements Modeling Projections Adaptive Optics Results Effects of Thermal

More information

Readout and control of a power-recycled interferometric gravitational wave antenna

Readout and control of a power-recycled interferometric gravitational wave antenna LASER INTERFEROMETER GRAVITATIONAL WAVE OBSERVATORY - LIGO - CALIFORNIA INSTITUTE OF TECHNOLOGY MASSACHUSETTS INSTITUTE OF TECHNOLOGY Publication LIGO-P000008-A - D 10/2/00 Readout and control of a power-recycled

More information

High Sensitivity Interferometric Detection of Partial Discharges for High Power Transformer Applications

High Sensitivity Interferometric Detection of Partial Discharges for High Power Transformer Applications High Sensitivity Interferometric Detection of Partial Discharges for High Power Transformer Applications Carlos Macià-Sanahuja and Horacio Lamela-Rivera Optoelectronics and Laser Technology group, Universidad

More information

Theory and Applications of Frequency Domain Laser Ultrasonics

Theory and Applications of Frequency Domain Laser Ultrasonics 1st International Symposium on Laser Ultrasonics: Science, Technology and Applications July 16-18 2008, Montreal, Canada Theory and Applications of Frequency Domain Laser Ultrasonics Todd W. MURRAY 1,

More information

Mystery noise in GEO600. Stefan Hild for the GEO600 team. 14th ILIAS WG1 meeting, October 2007, Hannover

Mystery noise in GEO600. Stefan Hild for the GEO600 team. 14th ILIAS WG1 meeting, October 2007, Hannover Mystery noise in GEO600 Stefan Hild for the GEO600 team 14th ILIAS WG1 meeting, October 2007, Hannover Intro: What is mystery noise? There is a big gap between the uncorrelated sum (pink) of all known

More information

VELA PHOTOINJECTOR LASER. E.W. Snedden, Lasers and Diagnostics Group

VELA PHOTOINJECTOR LASER. E.W. Snedden, Lasers and Diagnostics Group VELA PHOTOINJECTOR LASER E.W. Snedden, Lasers and Diagnostics Group Contents Introduction PI laser step-by-step: Ti:Sapphire oscillator Regenerative amplifier Single-pass amplifier Frequency mixing Emphasis

More information

Stability of a Fiber-Fed Heterodyne Interferometer

Stability of a Fiber-Fed Heterodyne Interferometer Stability of a Fiber-Fed Heterodyne Interferometer Christoph Weichert, Jens Flügge, Paul Köchert, Rainer Köning, Physikalisch Technische Bundesanstalt, Braunschweig, Germany; Rainer Tutsch, Technische

More information

Noise Budget Development for the LIGO 40 Meter Prototype

Noise Budget Development for the LIGO 40 Meter Prototype Noise Budget Development for the LIGO 40 Meter Prototype Ryan Kinney University of Missouri-Rolla, Department of Physics, 1870 Miner Circle, Rolla, MO 65409, USA Introduction LIGO 40 meter prototype What

More information

Seismic Noise & Vibration Isolation Systems. AIGO Summer Workshop School of Physics, UWA Feb Mar. 2, 2010

Seismic Noise & Vibration Isolation Systems. AIGO Summer Workshop School of Physics, UWA Feb Mar. 2, 2010 Seismic Noise & Vibration Isolation Systems AIGO Summer Workshop School of Physics, UWA Feb. 28 - Mar. 2, 2010 Seismic noise Ground noise: X =α/f 2 ( m/ Hz) α: 10-6 ~ 10-9 @ f = 10 Hz, x = 1 0-11 m GW

More information

Evaluation of Scientific Solutions Liquid Crystal Fabry-Perot Etalon

Evaluation of Scientific Solutions Liquid Crystal Fabry-Perot Etalon Evaluation of Scientific Solutions Liquid Crystal Fabry-Perot Etalon Testing of the etalon was done using a frequency stabilized He-Ne laser. The beam from the laser was passed through a spatial filter

More information

Experimental Physics. Experiment C & D: Pulsed Laser & Dye Laser. Course: FY12. Project: The Pulsed Laser. Done by: Wael Al-Assadi & Irvin Mangwiza

Experimental Physics. Experiment C & D: Pulsed Laser & Dye Laser. Course: FY12. Project: The Pulsed Laser. Done by: Wael Al-Assadi & Irvin Mangwiza Experiment C & D: Course: FY1 The Pulsed Laser Done by: Wael Al-Assadi Mangwiza 8/1/ Wael Al Assadi Mangwiza Experiment C & D : Introduction: Course: FY1 Rev. 35. Page: of 16 1// In this experiment we

More information

High performance vibration isolation techniques for the AIGO gravitational wave detector

High performance vibration isolation techniques for the AIGO gravitational wave detector High performance vibration isolation techniques for the AIGO gravitational wave detector Eu-Jeen Chin 2007 This thesis is presented for the degree of Doctor of Philosophy of The University of Western Australia

More information