How to Build a Gravitational Wave Detector. Sean Leavey

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1 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

2 Gravitational Wave Interferometry Sean Leavey How to Build a Gravitational Wave Detector 2/26

3 How to Build a GW Interferometer I am working on... ETMY Technical noise sources Actuation upon cavity mirrors Arm Cavity Y ITMY New topologies EOM PRM BS Arm Cavity X Interferometer control ITMX SRM ETMX PD Sean Leavey How to Build a Gravitational Wave Detector 3/26

4 How to Build a GW Interferometer Part 1 Mitigating technical noise Technical Infrastructure Materials and mirrors Interferometer topology Make it Quiet Fundamental noise sources Technical noise sources Control Systems Test mass actuation Control schemes Sean Leavey How to Build a Gravitational Wave Detector 4/26

5 Technical Noise Sources The interferometer needs to be quieter than the thing you want to measure Thermal noise in mirrors and suspensions Seismic noise around the site Electronic noise in controllers and readout Others: laser noise, oscillator noise, gravity gradient noise, and more... Strain [1/ Hz] Quantum noise Seismic noise Suspension thermal noise Coating Brownian noise Substrate Brownian noise Total noise Frequency [Hz] Figure : Advanced LIGO noise (arxiv: ) Sean Leavey How to Build a Gravitational Wave Detector 5/26

6 Dielectric Mirrors n high n low n high Current detectors use dielectric mirrors Many (25-40) layers used to produce high reflectivity Each layer contributes thermal noise to signal (Jointly) limits current generation detectors at some frequencies Sean Leavey How to Build a Gravitational Wave Detector 6/26

7 Consider Waveguide Mirrors Almost coating-free, thus reducing thermal noise However, gratings introduce noise in a different way, coupling seismic and thermal noise into the GW channel Waveguide mirrors should, in theory, cancel this additional noise term, but no experimental verification existed... constructive interference grating structure waveguide (n high ) substrate (n low ) destructive interference Sean Leavey How to Build a Gravitational Wave Detector 7/26

8 Waveguide Mirrors Slow feedback (temperature) 1064 nm Fast feedback laser (PZT) Mode Frequency stabilisation servo Mixer 70 Hz sources 10 MHz cleaning fibre EOM CCD camera...so we conducted an experiment in Glasgow to quantify this additional noise. source Data acquisition system 10m Fabry-Perot cavity Using the 10 m prototype facility, we built an optical cavity to measure this sidemotion effect. RF Photodiode Sean Leavey How to Build a Gravitational Wave Detector 8/26

9 Waveguide Mirrors Measurement uncertainty made it difficult to quantify the exact level of coupling, but it is orders of magnitude better than grating mirrors in terms of noise performance. Probability Density [arbitrary units] Transverse to Longitudinal Coupling [m / m] 1e 5 This work shows it might be possible to use these mirrors in future detectors to reduce thermal noise. Sean Leavey How to Build a Gravitational Wave Detector 9/26

10 How to Build a GW Interferometer Part 2 Low noise actuation Technical Infrastructure Materials and mirrors Interferometer topology Make it Quiet Fundamental noise sources Technical noise sources Control Systems Test mass actuation Control schemes Sean Leavey How to Build a Gravitational Wave Detector 10/26

11 Operating Point A GW interferometer needs to be at its operating point to be optimally sensitive, with each mirror s position controlled to within as little as m. Operating Point (Roughly speaking) when each cavity within the interferometer is on resonance. Amplitude Waves i.e. each cavity fits an integer number of half-wavelengths. Sean Leavey How to Build a Gravitational Wave Detector 11/26

12 Actuation Cavities are kept on resonance by various means... (Slightly) change the laser s wavelength Slow feedback (temperature) Fast feedback (PZT) Frequency stabilisation servo 1064 nm laser Use voice coils and magnets on suspended optics and reaction masses Both are susceptible to certain types of environmental noise and technical challenges Sean Leavey How to Build a Gravitational Wave Detector 12/26

13 Electrostatic Drives For low noise actuation directly on the test mass, electrostatic drives are used. These are low range but low noise actuators. However, these introduce clipping losses due to the need to attach a pattern of conductive material onto the mirror. Sean Leavey How to Build a Gravitational Wave Detector 13/26

14 Electrostatic Drives Another design, shown in simulations, is to use a plate capacitor arrangement. This has not yet been demonstrated experimentally... Credit: Wittel et. al. (arxiv) Sean Leavey How to Build a Gravitational Wave Detector 14/26

15 Electrostatic Drives But we are currently building an experiment in Glasgow to demonstrate the plate capacitor concept. We hope to have results from this experiment in September Input Optics Aux1 Aux4 ESD Aux2 Aux Sean Leavey How to Build a Gravitational Wave Detector 15/26

16 How to Build a GW Interferometer Part 3 Make it quieter than ever before Technical Infrastructure Materials and mirrors Interferometer topology Make it Quiet Fundamental noise sources Technical noise sources Control Systems Test mass actuation Control schemes Sean Leavey How to Build a Gravitational Wave Detector 16/26

17 The Standard Quantum Limit Radiation Pressure Noise h RP (f ) = 1 P mf 2 L 2π 3 cλ Shot Noise h S (f ) = 1 L cλ 2πP Sean Leavey How to Build a Gravitational Wave Detector 17/26

18 Beating the Standard Quantum Limit Displacement measurements are subject to Heisenberg s Uncertainty Principle. Thus: and [ˆx (t), ˆx (t + δt)] 0 [ˆx (t), ˆp (t)] 0 However, momentum, which manifests itself as the speed at which a test mass moves, does commute: [ˆp (t), ˆp (t + δt)] = 0 Figure : John von Neumann. By LANL [Public domain], via Wikimedia Commons Sean Leavey How to Build a Gravitational Wave Detector 18/26

19 Cancellation of Radiation Pressure Noise It turns out that a zero-area Sagnac interferometer topology is automatically a speed-meter. We can use it to cancel radiation pressure noise. Sean Leavey How to Build a Gravitational Wave Detector 19/26

20 Possible Sensitivity Improvement Displacement [m/sqrt(hz)] Michelson Sagnac A factor of 10 improvement in sensitivity allows detectors to sense a factor 1000 more volume of our universe Frequency [Hz] Sean Leavey How to Build a Gravitational Wave Detector 20/26

21 The Glasgow Speed-Meter Experiment In vacuum, seismically isolated 1 g and 100 g cavity mirrors Electrostatic drives for direct actuation on test masses 0.5 M9 M12 M13 M3b 0.0 M5 M11 LaserStab M6 M14 input beam M1b M4 M8 M7 M10 M1a PhD3 M16 M3a M2b M15 PhD4 M2a Sean Leavey How to Build a Gravitational Wave Detector 21/26

22 Work So Far Various technical and scientific aspects have been considered so far... Coil drivers Electronic wiring Vacuum infrastructure Noise budgeting Lock acquisition Five year experiment = lots of work! Displacement equivalent noise [m / sqrt(hz)] Frequency [Hz] Quantum Noise Suspension Thermal Noise Coating Brownian Noise Thermooptic Noise Substrate Brownian Noise Residual Gas Noise Classical Sum Sean Leavey How to Build a Gravitational Wave Detector 22/26

23 How to Build a GW Interferometer Technical Infrastructure Materials and mirrors Interferometer topology Part 4 Control it Make it Quiet Fundamental noise sources Technical noise sources Control Systems Test mass actuation Control schemes Sean Leavey How to Build a Gravitational Wave Detector 23/26

24 Low Frequency Control The speed-meter s velocity response vanishes at low frequencies, so new control techniques are required Response BHD SSM M9 PDH Cavity A Carrier RF sidebands Signal sidebands Arm B PDH W / m / sqrt(hz) BHD Arm A Frequency (Hz) Sean Leavey How to Build a Gravitational Wave Detector 24/26

25 FI Sensing and Control Advanced LIGO Interferometric Control Scheme J. Kissel, for the ISC Group TMSY G v3 DARM α MICH ERM Laser ϕ m ~40 khz ~100 Hz CARM High Bandwidth Cavity Length Control Signal High Bandwidth Cavity Angular Control Signal FI MC3 MC1 PRM? Test Mass Quad Sus (QUAD) Beam Splitter / Fold Mirror Triple Sus (BSFM) HAM Large Triple Sus (HLTS) HAM Small Triple Sus (HSTS) Transmission Monitor Double Sus (TMTS) Output Mode Cleaner Double Sus (OMCS) Faraday Single Sus (OFIS) HAM Auxiliary Single Sus (HAUX) PR3 Input Mode Cleaner Power Recycling Cavity MCPY ~1 Hz MICH ~20 Hz PRCL ~20 Hz SRCL ~20 Hz MC2 PR2 Output Mode Cleaner ITMY CP BS ITMX CP SR2 Signal Recycling Cavity SR3? DC PD ETMY SR3 ~10 Hz SRM ~200 Hz CommHard, DiffHard, CommSoft, DiffSoft, ~10 Hz β SCRL ERM TMSX ETM X Sensing and control is a complicated business, even for standard topologies! Work on the speed-meter s control scheme is on-going. HAM Tip-Tilt Single Sus (HTTS) Credit: Jeff Kissel (LIGO-G ) Sean Leavey How to Build a Gravitational Wave Detector 25/26

26 Thanks for listening! Sean Leavey How to Build a Gravitational Wave Detector 26/26

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