G O D D A R D S P A C E F L I G H T C E N T E R 1 GW Interferometry at Goddard Space Flight Center...
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Transcript of G O D D A R D S P A C E F L I G H T C E N T E R 1 GW Interferometry at Goddard Space Flight Center...
![Page 1: G O D D A R D S P A C E F L I G H T C E N T E R 1 GW Interferometry at Goddard Space Flight Center Jordan Camp NASA / Goddard Space Flight Center Jan.](https://reader035.fdocuments.in/reader035/viewer/2022070407/56649e305503460f94b20b5f/html5/thumbnails/1.jpg)
1G O D D A R D S P A C E F L I G H T C E N T E R
GW Interferometry at Goddard Space Flight Center
Jordan CampNASA / Goddard Space Flight Center
Jan. 20, 2005
LIGO-G050038-00-Z
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2G O D D A R D S P A C E F L I G H T C E N T E R
This TalkThis Talk
•Frequency stabilization of lasers– Optical cavity– Molecular iodine
•Suspension point interferometer (SPI) for testing of low-frequency interferometry
•A few “politically correct” slides– New science direction for NASA
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3G O D D A R D S P A C E F L I G H T C E N T E R
Interferometry in SpaceInterferometry in Space
• Space interferometry a strategic direction in astronomy
• NASA and ESA are planning a significant number of space interferometry missions
– SIM 2010 Stellar interferometry – LISA 2014 Gravitational Waves– TPF-C 2015
TPF 2020 Extra-solar terrestrial planetsDarwin 2020
– MAXIM 2025 Black Hole imager (x-rays)– Etc…
• Need frequency stabilized lasers for all of these…
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4G O D D A R D S P A C E F L I G H T C E N T E R
LISA – Search for Gravitational WavesLISA – Search for Gravitational Waves
• A variety of astrophysical phenomena produce low-frequency gravitational waves– Massive BH binary
coalescence– Massive BH capture of
stellar mass BH– Galactic compact
binaries
•LISA will measure strain from GW’s of 10-21
•Measure position to 10-12 m, spacecraft separation of 5 x 109 m
• / ~ 10-21 for stabilized laser
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5G O D D A R D S P A C E F L I G H T C E N T E R
Methods of Laser StabilizationMethods of Laser Stabilization
• Frequency stabilization is only as good as the stability of the reference
• Optical resonator – Low-loss mirrors held fixed by ULE cavity– Length of cavity determines resonant
frequency– Variable DC frequency, temperature sensitive
• Atomic or molecular gas transition– Gas held in transparent cell– Transition provides absolute frequency
reference– Better at low frequencies, worse at high (~ 1
mHz crossover)
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6G O D D A R D S P A C E F L I G H T C E N T E R
Optical Cavities: experimental set-up Optical Cavities: experimental set-up
LaserIsolator
EOM
Cavities in 5 layers of gold Cavities in 5 layers of gold coated stainless steel in coated stainless steel in
vacuum chambervacuum chamber
Macor standoffs
Cavities manufactured from ULE Cavities manufactured from ULE cylinders with fused silica mirrors cylinders with fused silica mirrors optically contacted to end facesoptically contacted to end faces
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7G O D D A R D S P A C E F L I G H T C E N T E R
Results (Mueller, McNamara)Results (Mueller, McNamara)
ServoServoCrossoversCrossovers
LISA frequency noise requirementLISA frequency noise requirement
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8G O D D A R D S P A C E F L I G H T C E N T E R
Thermal noise limit to cavity frequency stabilization (K. Numata)
Thermal noise limit to cavity frequency stabilization (K. Numata)
•Thermal noise is fundamental limit to cavity stability
• Mechanical loss of spacer, mirror, coatings causes thermal noiseLimit ~ 3 Hz / Hz1/2 1 mHz
10-2 Hz / Hz1/2 100 Hz
NIST and VIRGO data both limited by ULE mirror substrates (Q ~ 6 x 104)
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9G O D D A R D S P A C E F L I G H T C E N T E R
Iodine laser stabilization layoutIodine laser stabilization layout
Laser
Laser
FI
FI
PP-MgO:LN
PP-MgO:LN
AOM
AOM
Iodine
Iodine
19 MHZ EOM
21 MHZ EOM
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10G O D D A R D S P A C E F L I G H T C E N T E R
Iodine stabilization laboratory setupIodine stabilization laboratory setup
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11G O D D A R D S P A C E F L I G H T C E N T E R
Iodine noise performance(20 cm length cell) V. LeonhardtIodine noise performance(20 cm length cell) V. Leonhardt
Intensity
Temperature
Electronic
0.0001 0.001 0.01 0.1Frequency [Hz]
1
10
100
1000
10000
lock-in amplifiert-noise sys1t-noise sys2ampl. sys2 probeampl. sys1 probefrequency noise
Absolute frequency
Insensitive to alignment and temperature
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12G O D D A R D S P A C E F L I G H T C E N T E R
Low-Frequency Interferometry TestbedLow-Frequency Interferometry Testbed
Suspension Point Interferometer testing platform
•goal: lock platforms at picometer, nanoradian level•stable platforms will allow study of interferometry, noise
Iodine stabilized laser
Iodine stabilized laser
Hexapod PZT actuator
IFO output
IFO output
“Stabilization (locking)” beam
“Evaluation (measurement)” beam
Stability information
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13G O D D A R D S P A C E F L I G H T C E N T E R
Suspension Point InterferometerSuspension Point Interferometer
Hexapod: 6 PZT’s for 6 DOF controlres ~ 230 Hz, Q ~ 62 iodine stabilized lasers:
sense/control hexapod, and measure residual noise
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14G O D D A R D S P A C E F L I G H T C E N T E R
SPI Performance so farSPI Performance so far
10-15
10-14
10-13
10-12
10-11
10-10
RM
S S
ensi
ng
No
ise
[m]
0.0001 0.001 0.01 0.1 1
Frequency[Hz]
10-13
10-12
10-11
10-10
10-9
10-8
Dis
pla
cem
ent
No
ise
[m/r
tHz]
0.01 0.1 1 10 100 1000
Frequency[Hz]
Measurement system noise
Actuator noise
Sensor noise
Closed loop stability
Next: use ULE and bonded optics
Stability limited by CTE of mechanical mounts
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15G O D D A R D S P A C E F L I G H T C E N T E R
New direction for NASA scienceNew direction for NASA science
• “We support NASA’s Vision for Space Exploration….”– Moon, mars, infinity and beyond….
• Science activities shifting in this direction– Earth science measurements to support
planetary science of Mars, Saturn, etc.– Astrophysics must also show relevance to this
(not easy…)
• Terrestrial planet finding now a hot subject
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16G O D D A R D S P A C E F L I G H T C E N T E R
TPF – C : Search for Terrestrial PlanetsTPF – C : Search for Terrestrial Planets
•Coronagraph will look for reflected light from planet by blocking direct star light from nearby stars (< 15 pc)
•Spectroscopy of signal will give information on composition of planetary atmosphere
•Water, CO2, methane
•Contrast ratio of 1 : 109
•Telescope stability is very important
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17G O D D A R D S P A C E F L I G H T C E N T E R
Interferometry in TPF-CInterferometry in TPF-C
Stabilized laser and hexapod will control secondary mirror to10-9 m, 10-9 radian over hour timescaleMetrology and control scheme will be developed on SPI
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18G O D D A R D S P A C E F L I G H T C E N T E R
SummarySummary
• Stabilized lasers will fly!– LISA 2013– TPF-C2014
• Optical resonator and molecular transition under study– Noise requirements– Space qualification
• SPI testbed for low-frequency space interferometry – Iodine stabilization most useful