Phasemeter development for LISA at JPL · 2016. 3. 29. · Sept 10, 2011 – Dec 17, 2012 Gravity...
Transcript of Phasemeter development for LISA at JPL · 2016. 3. 29. · Sept 10, 2011 – Dec 17, 2012 Gravity...
Jet Propulsion Laboratory California Institute of Technology
Phasemeter development for LISA at JPL
Bill Klipstein, Kirk McKenzie
Brian Bachman, Jeff Dickson, Bob Spero, Brent Ware, Chris Woodruff
JPL LISA Interferometry Test bed
Built to prove the LISA Phasemeter LISA (-lite) Phasemeter delivered as part of the
GRACE Follow-On Laser-Ranging Interferometer
Jet Propulsion Laboratory California Institute of Technology
Laser Frequency Stabilization via Spatial Mode Interference
(Tilt-Locking)
Kirk McKenzie (335B)
Glenn de Vine (335B), Robert Thompson (332J), Robert Spero (383A), Daniel
Shaddock (ANU), William Klipstein (335), Brent Ware (383H)
Division 33 Staff Presentation, June 5th 2012
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Laser Interferometer Space Antenna
GRACE follow-on laser ranging instrument
Preliminary instrument specifications
Prepared by: Benjamin Sheard, Gerhard Heinzel
Checked by: Frank Flechtner
Document reference: GFO-LRI-AEI-RS
Version: 1.3
Date: February 22, 2012
Albert Einstein Institute, Hannover GeoForschungsZentrum, Potsdam
GRACE Follow-On
Funded via the CIF program
Gravity-Sensing Instruments in Space
Gravity Recovery and Interior Laboratory (GRAIL),
Planetary science, microwave measurements (micrometers)
Sept 10, 2011 – Dec 17, 2012
Gravity Recovery and Climate Experiment (GRACE),
Earth Science, microwave measurements (micrometers)
2002-present.
Laser Interferometer Space Antenna (LISA)
Astrophysics, (picometers)
ESA Cosmic Visions L3 (2034)
GRACE Follow-On
Earth Science,
Microwave (micrometers), Laser (nanometers)
Laser Ranging Interferometer as Joint US-German instrument
Aug, 2017 launch
Microwave Instrument ~ Micrometer Precision
Laser Instrument ~ Nanometer to Picometer Precision
Jet Propulsion Laboratory California Institute of Technology
OBE
DWS
FSM
Df=f1-fC1
q
Laser(f1)
Phase Lock
Cavity(fC1)
DWS
FSM
Laser(f1)
Pointing Control
OBE Cavity(fC2)
Df=f2-fC2
Phase Lock
Pointing Control
Frequency Stabilization
OBA
Frequency Stabilization
LRI 2
TMA TMA
LRI 1
dL
~200 km
10 Hz data
to GND
10 Hz data
to GND
LRP
LRP
OBA
The LRI is a (highly successful) partnership between the US and Germany*
• US (NASA/JPL): Phasemeter, Laser, and Optical Cavity,
Germany (AEI, DLR, STI: Optical Bench, Photodetectors, Triple Mirror
Assembly, Baffles
• LRI Phasemeter was design based on LISA technology and capabilities
• LISA/LRI have similar
• Phase tracking/signal readout
• Received optical power
• Lasers
• Photodetectors
• Laser frequency control (phase locking and frequency stabilization)
The Phasemeter has natural interfaces to Partner’s payload elements
The Laser Ranging Interferometer (LRI)
on GRACE Follow-On
*- see partner list on last slide
Jet Propulsion Laboratory California Institute of Technology Basics of LISA Interferometry
• LISA optical beat note ranges from 2 MHz - 20 MHz due to Doppler shift from
spacecraft velocity.
• One wavelength shift in one optical field produces a one cycle shift in the beat
note.
• The phasemeter measures the science signal as a milliHertz phase modulation
on a megahertz beat signal.
• LISA has uneven arm lengths – Time Delay Interferometry (TDI) needed to
synthesis a equal arm length interferometer
– Phasemeter tracks “noisy” beatnotes and sends data to
ground.
– Algorithm of delayed phasemeter signal enables
cancellation of laser frequency noise (common to both
interferometer arms) leaving gravitational wave signal
(differential signal).
f1
f2 fbeat = f1 - f2
Photodetector
Time Delay
Interferometry
TDI Science Phasemeter
Data to
ground
Jet Propulsion Laboratory California Institute of Technology All functions of the Phasemeter at
TRL 4 or Flight
• The phasemeter core functionality:
– Produces science data (interferometer readout)
– Offset phase locks the slave laser to the received laser light
– Stabilizes the master laser to the frequency reference (cavity)
– Derives differential wavefront sensing signals for laser pointing
– Measures “clock sidebands” for USO noise cancellation
– Measures inter-spacecraft separation to 1m absolute accuracy to
facilitate Time Delay Interferometry
• All above functions have been demonstrated at TRL 4/5 or above for
LISA required levels.
• Blue functions have been demonstrated at TRL 9 (FLIGHT) for LRI
(some performance requirements not tested to LISA levels – e.g.
phase locking – due to relaxed requirements for LRI)
Jet Propulsion Laboratory California Institute of Technology
6
“Phasemeter” Naming of parts
Quadrant photoreceiver
converts laser beat note
into electrical signal
TRL: 4/5 (LISA)
FLIGHT (LRI)
Amplifies and
digitizes analog
signal
TRL: 4 (LISA)
FLIGHT (LRI)
Provides stable timing
for ADC sampling
Not a technology
development required
FLIGHT (GRAIL)
Multiplies USO signal to
programmable value to drive
laser phase modulator:
FLIGHT (GRAIL heritage)
HEART OF THE PHASEMETER:
Digital phasemeter measures phase,
controls laser frequency, and
generates timing/ranging signals:
approaching TRL 5/6
FLIGHT (LRI) Processor back-
end: TRL 4 (LISA)
FLIGHT (LRI)
Performance in LISA interferometer testbed demonstrates system at TRL 4
Jet Propulsion Laboratory California Institute of Technology
Time Delay Interferometry with the LISA
Phasemeter JPL LISA interferometer testbed built to demonstrate the phasemeter
and measurement system performance to TRL 4.
• Retired the highest LISA phase measurement risk1
• Frequency noise removal to interferometer displacement limit
• Clock Tone Transfer via GHz phase modulation
• Interpolation of data streams onto common time-base
1 NASA’s LISA Technology Development Plan V 1.0 ( 2005)
Upgrading to TRL5 with GFO HW
Jet Propulsion Laboratory California Institute of Technology
JPL LISA Interferometry Contributions
JPL LISA interferometry contributions since 1996:
• Time Delay Interferometry1 (1999)
• Post-processing interpolation TDI2 – TDI made practical on a spacecraft (2003)
• Development of Arm locking3,4 - Use LISA arms as frequency reference
• Velocity-correcting Time Delay Interferometry5 (2004)
• Demonstration of clock noise suppression6
• First experimental demonstration of TDI7 (2008)
• Invention of picometer phasemeter (US 7,511,469)
• Optical ranging to absolute accuracy to 0.2m rms8
• Optical Communications on the laser link (20 kbps)8
• Track very low light power (<3pW)
• Design of the GRACE Follow-On LRI9 (2012)
• Differential Wavefront Sensing Demonstrated
• Interferometer system engineering (US Co-Chair of Interferometry ITAT)
• Design of LISA TDI experiment for GRACE Follow-On LRI10
• Design of LISA Arm Locking experiment for GRACE Follow-On LRI11
• Developed Flight Cavity 12
• LISA Phasemeter on LRI
1 J. W. Armstrong, F. B. Estabrook, and M. Tinto, ApJ 527 814 (1999)
2 D. A. Shaddock, B. Ware, RE Spero, M Valisineri PRD (2004)
3 B. S. Sheard, M. B. Gray, D. E. McClelland, and D. A. Shaddock, Phys. Lett. A 320, 9 (2003).
4 K. McKenzie, R. E. Spero, and D. A. Shaddock, Phys. Rev. D 80 102003 (2009)
5 D.A. Shaddock et al PRD (2003)
6 W. Klipstein et al., AIP Conf. Ser. No. 873 (2006)
7 G. de Vine, B. Ware, K. McKenzie, R.E. Spero, W. M. Klipstein and D. A. Shaddock PRL (2010)
8 A. Sutton, K. McKenzie, B. Ware, and D. A. Shaddock OE (2010)
9 B. Sheard, G. Heinzel et al Journal of Geodesy . doi:10.1007/s00190-012-0566-3. (2012)
10 S. P. Francis, D. A. Shaddock, A. J. Sutton, et al Phys. Rev. D 92, 012005 (2015)
11 J. I. Thorpe, K. McKenzie accepted PRD 2016
12 W. M. Folkner, G. deVine, W. M. Klipstein, et al Earth Science Tech. Forum, (2010).
Jet Propulsion Laboratory California Institute of Technology
9
LRI Phasemeter is LISA-lite Phasemeter
TRL 4 unit stress tested in all-digital tests and in interferometer
testbed
GRACE Follow-On Laser Ranging Processor implements for flight
LISA phase tracking and frequency control algorithms, including:
• Phase tracking
• differential wavefront sensing (and control)
• Laser Phase Locking
• Laser frequency stabilization
• Multi-tone tracking to be added under SAT
• Has only 4 input channels (vs 18 for LISA)
Jet Propulsion Laboratory California Institute of Technology
LRI 1 at STI Immenstaad am Bodensee
LRP
LAS
TMA
OBA
OBE
CAV OGSE
Baffles
German
US
LRI Flight Hardware just prior to spacecraft integration
Jet Propulsion Laboratory California Institute of Technology
Laser Frequency Stabilization Using Flight
Phasemeter with flight Cavity and Laser (LRI-US)
GRACE-FO LRI PDR DRR GFO-13-071
10a-4
30May2013
Jet Propulsion Laboratory!California Institute of Technology!
Cavity Assembly Program
Overview
The technical data in this document is controlled under the U.S. Export Regulations; release to foreign persons may require an export authorization.
• Cavity assembly design quite mature based on NASA
Instrument Incubator Program investment (2008-2011) and
continued work in Phase A, and B!
• Two breadboard units in operation in JPL Testbed !
• Meets top level performance requirements with margin!
• Breadboard photodiode preamplifiers units built in phase A!
• Optical fiber routing mock-up completed!
• Long lead parts ordered at end of phase A!
• Optical fiber!
• Photodiode !
• ULE cavities!
Optical Cavity
• LRP implements laser frequency control
(locks laser to cavity assembly)
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RLU EQM phase 1
TV chamber
June 2013
RLU mounted in TV chamber
05.07.2013 6
• Similar to Laser on LISA Pathfinder
• Wavelength: 1064 nm
• Nd:YAG Non-Planar Ring Oscillator
• Laser output power: 25 mW +/- 20%
Laser
• Flight phasemeter controlling
flight laser to flight cavity, x2
GRACE-FO rqmt
LISA rqmt
Jet Propulsion Laboratory California Institute of Technology
• 1 mm diameter quadrant diode with pre-amp
• Meets performance requirements for noise and phase stability
Photoreceiver Prototype: TRL 4/5
12
Phase slope measurement
• Our LRI partners in Germany
(DLR, STI, AEI) developed a
similar design to FLIGHT for LRI
• GSFC investigated a hybrid
photoreceiver
Jet Propulsion Laboratory California Institute of Technology Analog-to-digital signal chain: TRL 4
• Amplifies, filters and digitizes signals from photoreceiver
quadrants
• 50 MSamples/S, 12 bits: not driving
• Includes sampling time jitter calibration tone from USO
• Demonstrated to TRL 4 in interferometer testbed with commercial
components
• Flight amplifier/filter chain built for LRI by German partners
(AEI, STI, DLR)
• Flight samplers included in LRP on GRACE-FO
13
Amplifier/filter chain developed for FLIGHT for GRACE-FO by
LRI partners in Germany (DLR, STI, AEI)
Jet Propulsion Laboratory California Institute of Technology Frequency Multiplier/synthesizer
• Purpose: produces synthesized microwave copy of USO
frequency to transfer noise via light
– Used to measure and correct for clock noise
– Technique demonstrated in our testbed with “USO” 100x worse
than a USO1
– Requirements met by GRAIL radio science beacon
• Easily meets LISA requirements (requirements are off the charts)
14
fUSS= fDoppler – (fmod-f’mod)
fDoppler (<18 MHz)
Three unique frequencies
for modmod 'ff ¹
Using sideband-sideband beatnotes (instead of carrier-sideband) allows
high modulation frequency and low photoreceiver BW
~8 GHz
Science msrmt Lower clock msrmt upper clock msrmt
fLSS= fDoppler + (fmod-f’mod)
(1-2 MHz)
~
EOM
USO
X
fmod≈ 8 GHz
Laser
(to distant S/C)
1
9.901 103-
´
llii
100
æçè
ö÷ø
1 103
´1- 103
´ ii
ii 2000- 1999-, 2000..:=
llii
100
æçè
ö÷ø
ii
ii 2000- 1999-, 2000..:=
llii
100
æçè
ö÷ø
ii
(from other S/C)
fmod
f’mod
ADC
1 W. Klipstein et al., AIP Conf. Ser. No. 873 (2006)
Jet Propulsion Laboratory California Institute of Technology
15
Ultra-stable oscillator
USO provides a reference for the ADCs in the
phasemeter
• flight USOs exist (GRAIL shown). LISA does
not need state-of-the-art performance. This is
just a procurement
• On GRAIL the RSB (prev. slide) used one USO
output
1.0E-14
1.0E-13
1.0E-12
1.0E-11
1.0E-10
1.0E-09
1E-1 1E+0 1E+1 1E+2 1E+3 1E+4 1E+5 1E+6
All
an
de
via
tio
n s
y(t
)
t (seconds)
GRAIL USO-0901 vs. maser
GRAIL USO-1902 vs. maser
Jet Propulsion Laboratory California Institute of Technology GFO LRI Team
Tesat Daniel Troendle Steve Windisch Juergen Schaeufler Felix Kern Steffi Gross Iris Rock Reinhard Baehring Mustafa Cilo Simon Braeuchle Bjoern Siebertz Rudolf Bauer Hanno Scheife Claus Seibert Christoph Seiter
Ball Michelle Stephens Bob Pierce Bengie Amparan Gretchen Reavis Mike Sileo Dave Bender Mike Comstock Tracy Copp Amanda Curry Mike Davis Larry Derouin Michael Hoppes Jim Howell Carl Hunsaker Ken Jackson Paul Kaptchen Jim Leitch Aaron Mann Mark Neitenbach Tammy Osborne Mike Taylor
Photline
Philippe LeRoux
Houda Brahimi
Pascal Blind
Vincent Buin
Fatima Oruci
Jerome Hennemann
JPL
Bill Klipstein
Bob Spero
Brent Ware
Serge Dubovitsky
Alex Abramovici
Greg Rosalia
Marty Scarbrough
Christian Liebe
Tony Sherrill
Glenn de Vine
Kirk McKenzie
Andrew Sutton
Jeff Dickson
Brian Bachman
Alex Murray
Chris Woodruff
Yutao He
Ken Clark
David Barr
Mark Katsumura
Kameron Larsen
Jehhal Liu
Max Bize
Mike Burke
Joseph Trinh
Doug Wang
Josh Ravich
Omid Ghassemi
Greg Taylor
Don Nguyen
Tony Grata
Rick Paynter
Valereen Essandoh
Bill Folkner
Rabi Wang
Daniel Shaddock
Peter Halverson
ANU Daniel Shaddock Roland Fleddermann Robert Ward Danielle Wuchenich
AEI
Gerhard Heinzel
Ben Sheard
Christoph Mahrdt
Vitali Müller
Daniel Schütze
Gunnar Stede
Alexander Görth
Germán Fernández Barranco
LRI
Dennis Weise
Reinhold Flatscher
Simon Doerr
Cassidian - TMA Georg Luichtel Roswitha Keppeler Malte Schwarzer Martin Hinz Marcus Zimmermann Gerhard Dersch Gerhard Reile
DLR - QPR Andreas Eckardt Thomas Mangoldt Bernd Zender Burkhardt Guenther Thomas Lieder Josep Sanjuan Martin Gohlke Claus Braxmaier
Apcon - OBE Anton Lebeda Arnold Lebeda
STI
Frank Gilles
Kolja Nicklaus
Kai Voss
Rudolf Faimann
Manfred von Hoegen
Melanie Grossnick
Mark Herding
Timo Liebherr
Anne Götz
Marina Dehne
Vadim Pflug
Christian Diekmann
Andreas Baatzsch