Optical lever for KAGRA
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1 Optical lever for KAGRA Kazuhiro Agatsuma 2014/May/ /May/16 GW monthly seminar at Tokyo 1
2 Contents Optical lever (OpLev) development for KAGRA What is the optical lever? Review of OpLev in TAMA-SAS Requirements of KAGRA Selection of components Layout Performance test Toward bkagra (cryo-condition) 2014/May/16 GW monthly seminar at Tokyo 2
3 What is the optical lever? 2014/May/16 GW monthly seminar at Tokyo 3
4 OpLev is an angular sensor used for Local angular control of each mirror => to help lock acquisition of the interferometer Monitoring drift motion Position sensor Light source mirror 2014/May/16 GW monthly seminar at Tokyo 4
5 Principle Optical lever Position sensor Light source mirror c.f. Lever The mirror angle is increased by the distance of detection Load Effort L Fulcrum The effort force is reduced by the distance of effort arm Archimedes "Give me a place to stand and I will move the earth! ( 2014/May/16 GW monthly seminar at Tokyo 5
6 Objectives To decide detail design of OpLev Engineering test (prototype test) Position sensor Light source mirror OpLev looks easy! It looks a kind of LEGO. Does it need to research? => Yes. Operation is easy but suitable setup is not obvious to meet requirements (angular spectrum, drift, range) easy maintenance (easily available) reasonable price (10-20 OpLevs will be used) => suitable operation is achieved by accumulation of experiences 2014/May/16 GW monthly seminar at Tokyo 6
7 Review of OpLev in TAMA-SAS (Actual examples) 2014/May/16 GW monthly seminar at Tokyo 7
8 OpLev in TAMA-SAS TAMA-SAS Position sensor: QPD (quadrant photo diode) (2002, TAMA project report) 2014/May/16 GW monthly seminar at Tokyo 8
9 Sensitivity There were some exercises to reach the left sensitivity windshield laser angle cabling etc 2014/May/16 GW monthly seminar at Tokyo 9
10 Angular control by OpLev Mirror angular motion was suppressed by OpLev control (master thesis of K.A.) 2014/May/16 GW monthly seminar at Tokyo 10
11 KAGRA requirements 2014/May/16 GW monthly seminar at Tokyo 11
12 Requirement (spectrum) To lock IFO RMS: 0.1 urad (for cavity) RMS: 1 urad (for BS mirror) Requirement Intensity noise, shot noise ( ) In this calculation, following parameters are assumed Intensity noise of light source: RIN ~ 1e-7 /rthz Shot noise or dark noise: ~1e-11 m/rthz (as the spot fluctuation) by Michimura and Sekiguchi, JGW document (2012/4/27) 2014/May/16 GW monthly seminar at Tokyo 12
13 Requirement (drift, range) Drift 3 km remaining fringe 3 cm To be locked by referring to optical lever 3 cm / 3km = 10 urad 10 urad/week? 10 urad/day? 10 urad/h? If commissioning phase is assumed => To hold fringe for a day Drift: 10 urad/day Range If the local control is failure (turned off), the suspension system is fluctuated To follow unstable condition Range: 1~10 mrad (according to VIRGO empirically) 2014/May/16 GW monthly seminar at Tokyo 13
14 Selection of components 2014/May/16 GW monthly seminar at Tokyo 14
15 Selection of components Light source SLD (Super Luminescent Diode) Center wave length: 670 nm Thermal control is included Power: 1 mw Collimator lens Beam-spot size: it affects the linear range and sensitivity mm for PSD (c.f. 2mm in case of aligo) Photo receiver PSD (Position Sensitive Detector) Φ: 9 mm x 9 mm 2014/May/16 GW monthly seminar at Tokyo 15
16 Light source Selected parameters Fiber coupled SLD: to avoid interference with a reflection from cladding Center of wave length: nm Visible is useful at the installation and commissioning phase Tradeoff with lifetime (switchable to IR SLD, which has longer lifetime) Power: 1 mw (mirror reflection of 20-50% is assumed) Thermal control (to avoid the mode hop) PM fiber (to keep polarization because of high incident angle) FC/APC (to avoid returning light) 2014/May/16 GW monthly seminar at Tokyo 16
17 Measured RIN and lifetime from LIGO document This is much lower than the requirement 2014/May/16 GW monthly seminar at Tokyo 17
18 Position sensor Performance has been checked for below candidates PSD (Position Sensitive Detector) Large linear dynamic range Low speed response Spot-size-independent sensitivity QPD (Quadrant Photo Detector) Small linear dynamic range High speed response Spot-size-dependent sensitivity ( Spot size affects the linear dynamic range) 2014/May/16 GW monthly seminar at Tokyo 18
19 Calibration factors PSD (Position Sensitive Detector) Φ: 9 mm x 9 mm X-Y stage Φ 2mm: linear range: 7mm Φ 0.5mm: linear range: 8mm PSD: 7 mm (Φ 2 mm) QPD: mm (Φ 2-6 mm) Sensitivity is independent on the spot size => easy adjustment Linear range of PSD (7mm) is much larger than that of QPD (0.5mm) 2014/May/16 GW monthly seminar at Tokyo 19
20 Launcher (collimator lens & mirror) Selected launcher Spot size is 1-2 mm with the working distance of 4m Adjustable-focus lens (good match with PSD) Initial steering mirror 2014/May/16 GW monthly seminar at Tokyo 20
21 Layout 2014/May/16 GW monthly seminar at Tokyo 21
22 Optical layout Position sensor Light source Length coupling θ mirror mirror Large θ causes length coupling mirror Turning mirror 2014/May/16 GW monthly seminar at Tokyo 22
23 Layout design Chamber for Type-B SAS Default Option 1 (Mixed signal) BS Range: 8mm/(2*1m) = 4 mrad Option 2 (Broad range & length) Turning port Input port BS lens PSD Range: 8mm/(2*3m) = 1.3 mrad 2014/May/16 GW monthly seminar at Tokyo 23
24 Turning port Option 1 (Mixed signal or Length information) Subtraction of angular signal (input port) from the mixed BS PSD output produces the longitudinal signal Merit: Cheap and simple Demerit: Direct coupling between longitudinal and lens angular motion Option 1.5 Option 2 (Broad range & Length) BS lens (Broad range or Length information) To adjust the focal or image plane by adding a lens PSD PSDs have to be placed on the focal plane and image plane using sliders with about 10-um accuracy Merit: Clear separation between longitudinal and angular motion Demerit: Extra optics (PSD, lens and their sliders) increase total cost. Option 1 Option 1.5 Option 2 Cost Low Middle High Information Mix or Length Broad or Length Broad and Length 2014/May/16 GW monthly seminar at Tokyo 24
25 Layout design for Type B (preliminary) Breadboard Drown by Gianni Gennaro 2014/May/16 GW monthly seminar at Tokyo 25
26 Performance test 2014/May/16 GW monthly seminar at Tokyo 26
27 Comprehensive drift (NAOJ) ~1m Thermometer Paper box was used as windshield PSD 2014/May/16 GW monthly seminar at Tokyo 27
28 Comprehensive drift (NAOJ) Fitting: Y = α + β*t + γ*(x t) T: temperature, β: temperature response x: time, γ: constant drift t: time delay To hold fringe for a day Drift: 10 urad/day X direction: β = 8 um/k, γ = 14 um/day => 2 urad/day Y direction: β = 50 um/k, γ = 170 um/day => 30 urad/day (3m OpLev length) Origin of this drift is in investigation 2014/May/16 GW monthly seminar at Tokyo 28
29 Comprehensive drift (Nikhef) ~1m Thermometer (Pt100) Windshield SLD PSD 2014/May/16 GW monthly seminar at Tokyo 29
30 Comprehensive drift (Nikhef) 25 min. Temperature control in lab. X direction: β = 44 um/k, γ = 6.4 um/day => 0.7 urad (0.1K/day in Kamioka) + 1 urad(drift) = 1.7 urad/day (OpLev length of 3m is assumed) Fitting function: Y = α + β T + γ (x t) T: temperature, β: temperature response x: time, γ: constant drift t: time delay Y direction: β = 600 um/k, γ = 13um/day => 10 urad (0.1K/day) + 2 urad(drift) = 12 urad/day (OpLev length of 3m is assumed) These results almost achieved the requirement of KAGRA (10 urad/day) 2014/May/16 GW monthly seminar at Tokyo 30
31 Comparison with NAOJ result Nikhef X NAOJ (talk at 2 nd ELiTES meeting) Y Condition is better than NAOJ all mirror use thread-pitch locks temperature is stable in the clean room heavy optical table metal windshield 2014/May/16 GW monthly seminar at Tokyo 31
32 Spectrum of spot fluctuation limited by digitization noise Thermal drift is seen below 0.1 Hz worse than X direction => mechanical vibrations Optical lever length of 3 m is assumed => divided by factor of 6 => ~ 1 nrad/rthz at 1 Hz 2014/May/16 GW monthly seminar at Tokyo 32
33 Intensity noise by offset (Blue line) Consistent with RIN measurement within difference factor of 2 (The left response has two times smaller RIN than the right graph shows) => an individual difference of SLD 2014/May/16 GW monthly seminar at Tokyo 33
34 Investigation of large thermal response The temperature response of Y direction is relatively worse: (X: β = 44 um/k, Y: β = 600 um/k) Table bending?? Short length setup Scaling factor only? Scaling factor + bending? 2014/May/16 GW monthly seminar at Tokyo 34
35 Investigation of large thermal response θ 2 d1 θ 3 θ 1 ( ) cm = (100.5) cm, d1 = 111 cm Optical path length: 449 cm OpLev length: 348 cm Return mirror OpLev: 244 cm ( ) cm = (14.5) cm, d2 = 29 cm Optical path length: 129 cm OpLev length: 114 cm Return mirror OpLev: 85 cm L spot = 2x(4.5xθ xθ xθ 3 ) S spot = 2x(1.3xθ xθ xθ 3 ) L spot /S spot = ~3: Scaling factor (θ 1 =θ 2 =θ 3 ) d1/d2 = 3.8 : Table deformation factor 2014/May/16 GW monthly seminar at Tokyo 35 d2 Which is the real factor? 3 (dominated by local mirrors) or 3x3.8=11 (dominated by table deformation)
36 Short length measurement X Y Short: β = 44 um/k, γ = 0.6 um/day x1 x10 (Long: β = 44 um/k, γ = 6.4 um/day) X temp: Translational motion of SLD or PSD X drift: Table bending dominant Fitting function: Y = α + β T + γ (x t) T: temperature, β: temperature response x: time, γ: constant drift t: time delay Short: β = 45 um/k, γ = 1.9 um/day x13 x7 (Long: β = 600 um/k, γ = 13 um/day) Y temp: Table bending dominant Y drift: Table bending dominant (almost) Expected drift (scaling factor: x3 for 3m length, 0.1 K/day) X: β = 44 um/k, γ = 2 um/day => ~1 urad/day Y: β = 150 um/k, γ = 6 um/day => ~3 urad/day 2014/May/16 GW monthly seminar at Tokyo 36
37 Next step Pylon 2014/May/16 GW monthly seminar at Tokyo 37
38 Toward bkagra (perspective for cryogenic system) 2014/May/16 GW monthly seminar at Tokyo 38
39 Layout test mass chamber for bkagra ~15 m test mass chamber for ikagra 2014/May/16 GW monthly seminar at Tokyo 39
40 Layout for ikagra OpLev length: 3m Optical path length: 4m Range: 8mm/(2*3m) = 1.3 mrad ~ 1 m Turning port Input port Pylon 2014/May/16 GW monthly seminar at Tokyo 40
41 Layout for bkagra OpLev length: 15 m Optical path length: 30 m ~ 15 m Range: 8mm/(2*15m) ~ 0.3 mrad! aligo Detection port Design of collimator lens will be needed Pylon Observable range becomes small (1.3 mrad => 0.3 mrad) 2014/May/16 GW monthly seminar at Tokyo 41
42 OpLev inside cryostat Merit inside cryostat Observing Intermediate mass Short length OpLev (broad range) Technical misc. No optical window Fiber coupled SLD is useful Cryo-compatible PD What should be the reference? - Cryostat => deformation by changing temperature - Making special pylon (super invar?) => difficult 2014/May/16 GW monthly seminar at Tokyo 42
43 Summary Selection and prototype test for the OpLev of ikagra Selection Laser source: Superlum SLD (670 nm) with PM fiber, Position sensor: PSD (9mm x 9mm), Collimator lens: Adjustable-focus lens is selected for PSD (Φ2 mm at 2-m WD, Φ1 mm at 4-m WD) Performance tests The comprehensive drifts are X:1 urad/day, Y: 3 urad/day The angular spectrum is 1 nrad/rthz at 1 Hz on an optical bench => Optical components are expected to achieve requirements Layout Current range (PSD, 8mm range, and input port) is 1.3 mrad for the angular motion of mirrors. It is useful to detect the signal at not only input port but also the turning port. (It is said that 10 mrad range is sufficient for SA in VIRGO) Perspectives Long-length OpLev have a high sensitivity but small range Additional OpLev inside cryostat has some merits (broad range and seeing intermediate mass) 2014/May/16 GW monthly seminar at Tokyo 43
44 Acknowledgements Riccardo DeSalvo Ettore Majorana Ryutaro Takahashi Tomotada Akutsu Takanori Sekiguchi all member of VIS, AOS, and QND group. 2014/May/16 GW monthly seminar at Tokyo 44
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