ligo lsc meeting march 19-23, 2006 interferometer sensing and control wg 1...
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![Page 1: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/1.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
LIGO Photodiode Development and Optical Platform for LIGO Photodetectors Testing
LSC March MeetingLIGO Hanford Observatory, March 22, 2006
Ke-Xun SunPhotodiodes --- with Rana Adhikari, Peter Fritschel,
Osamu Miyakawa, Allan Weinstein, David Jackrel, Brian LantzOptical Platform --- with Vern Sandberg, Fred Raab, Dick Gustafson
EOPM EOAM
EOPM EOAM
PBS
![Page 2: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/2.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
RF Singlet Detector for LIGO+ and Adv. LIGO
• Material: InGaAs based family
• Pattern: Single element
• Diameter > 2 mm
• Frequency response: ~100 MHz
• Packaging: rf operable
• Cooling: Possible TEC
• Optical power: ~1 W
• Quantum efficiency target: 70%
2 mm
![Page 3: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/3.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
RF Quad Detectors for LIGO+ and Advanced LIGO
• Material: InGaAs based family• Pattern: Quad (see options right)• Gap size > 100 m• Active receiving area: 1 cm2 span• Frequency response: >100 MHz• Cross talk: 6 dB Better than minimum SNR
– Neighbor: -20dB @ 100 MHz– Diagonal: -23 dB @ 100 MHz
• Packaging: Multi pin rf operable• Optical power: ~100 mW total• Quantum efficiency target: 70%• Other ideas (see right)
Arrayed single detectorsUse with lens arrays (commercially available)
Large gap quad photodiodes
![Page 4: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/4.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Commercial InGaAs Quad Photodiodes• Hamamatsu
– 6849-01 • 1 mm, 80 MHz
– 6849 • 2 mm, 30 MHz
– Cross coupling via the single cathode pin connection
A1
A3
A2
A4
C
![Page 5: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/5.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Back Illuminated Photodiodes for High Power Optical Detection
• “Flip over” to facilitate heat dissipation
• Improved transmittance in the “new front”
• Power level raised• Need device
packaging• Need RF packaging• Need systematic
testing
![Page 6: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/6.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Probe Testing Results
Data shown from D. Jackrel LSC 2005
The new 2006 strategy: Packaging and testing needs to be improved for high frequency applications
![Page 7: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/7.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Detector Work at Stanford
• Catalog existing chips from David
• Ordered 30 InGaAs chips
• Negotiating wire bonding
• RF packaging comparison
• External resonant elements
• Structure design to allow TEC cooling
• Look for a grad student
• Or an interactive commercial sensor
• (Commercial products?)
Verify the design first
![Page 8: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/8.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
RF Packaging of Quad Detector Options
• Use separate cathode pins• Add grounding ring and
grounding for – Better isolation
– External resonant circuits
• Use BGA pin fan out • Allow heat sink and TEC
cooling
A1
A4
A2
A3
C2
C1
C3
C4
A1 C1 G1 G2 C2 A2
A4 C4 G4 G3 C3 A3
![Page 9: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/9.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Optical Test Platform at LIGO HanfordSimulates all field components at all frequenciesCan be built step-by-by step to reduce cost shock
EOPM EOAM
EOPM EOAM
PBS
Laser
Isolator
BS2(PBS or NPBS)
EOPM
![Page 10: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/10.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Wavefront and Alignment Sensing
Wavefront sensor• RF modulation
– Phase – Amplitude
• Overlap modulation– Beam displacement (~4x103x(30/2)x10-17~ 0.6 pm)– Coherent (co-polarized fraction)– Incoherent (orthogonal polarized fraction)– Angular modulation
Alignment sensor– DC or lock-in amplifier (~100 kHz) frequency
LIGO beam pointing simulation
EOAM
EOAM
PZTs
PZTs
![Page 11: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/11.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Single Side Band Frequency Shift
Single side band frequency • Optical heterodyne frequency down shift for
advanced LIGO wavefront sensor (Peter Fritschel) – Down shift from 200 MHz to below quad
detector bandwidth– No beam movement– Tunable
• Double pass AO– Use an acoustic modulator (AO)– Curve mirror – Double pass for 2 modulation
EOPM
AO
![Page 12: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/12.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
A More Complete PlatformStep by step implementation
• Cavity Phase Shifter
• Frequency Shifter
Laser
Isolator EOPM EOAM
EOPM EOAM
PBS
BS2(PBS or NPBS)
AO
Cavity
![Page 13: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/13.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Orthogonally Polarized Local Oscillator
• Simulated amplitude noise by using Amplitude modulation
• CMRR >30 dB with adjustable gain amplifiers
![Page 14: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/14.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
Spectrum Measurement at 90.9 MHz Amplitude Noise Suppression 32 dB
Good for AS_I Mitigation?
![Page 15: LIGO LSC Meeting March 19-23, 2006 Interferometer Sensing and Control WG 1 LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. Sun LIGO-G060141-00-Z LIGO Photodiode](https://reader036.vdocuments.us/reader036/viewer/2022070413/5697bff71a28abf838cbec82/html5/thumbnails/15.jpg)
LIGO LSC Meeting March 19-23, 2006Interferometer Sensing and Control WG
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LIGO_LSC_Sun_Photodiode_060322v2.ppt, K. SunLIGO-G060141-00-Z
SummaryIterative Steps of Detector Development
1. System requirement
2. Chipset configuration
3. Material science
4. RF packaging
5. External matching circuit
6. Device testing
7. System testing