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