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~ 2015

~ 2015. 3 Mission specific challenges: Data Analysis GRS Interferometry. LISA vs. LIGO. LISA: Joint NASA/ESA project. LIGO: NSF project. Advanced LIGO. EMRIs. Generate realistic data streams for data analysis tests. Data Analysis Challenge: Can we identify all signals ?.

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~ 2015

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  1. ~ 2015 • 3 Mission specific challenges: • Data Analysis • GRS • Interferometry

  2. LISA vs. LIGO LISA: Joint NASA/ESA project LIGO: NSF project Advanced LIGO EMRIs

  3. Generate realistic data streams for data analysis tests

  4. Data Analysis Challenge: Can we identify all signals ?

  5. Data Analysis: Galactic Binary Routines

  6. Markov Chain Monte Carlo Simulations with simulated full data sets showed first successful results. Opportunities to get involved Testbed for LISA Analysis Mock LISA Data Challenge Lots to do many things to contribute … DA is progressing well Data Analysis Take Away

  7. LISA Gravitational Reference Sensors TeV Particle Astrophysics II University of Wisconsin, Madison, August 28-31, 2006 Ke-Xun Sun Stanford University For the LISA GRS Research Community

  8. GRS Gravitational Reference Sensor (GRS) in the LISA Spacecraft

  9. Sensitive path To and from Remote Spacecraft Waveplate Transmissive optics Proof Mass Proof Mass Baseline Design: Two Cubic Proof Masses per Spacecraft

  10. LISA Test Package: ESA Space mission to test the GRS • Performance Goal: • Acceleration < 10-14m/s-2/3 (10 times LISA) • Understand the system Launch: 2009!

  11. LISA Noise Sources Additional leading term: Voltage Reference Instability

  12. Incoming Laser Beam Outgoing Laser Beam Telescope GRS Housing Details Shown in Figure 2 Optical Readout Beam Large gap Proof Mass Alternative Single PM Design Sun, Allen, Buchman, DeBra, Byer, CQG (22) 2005 S287-S296

  13. GRS Take away: LISA Test Package: ESA Space mission to test the GRS Launch: 2009 • Two inertial sensors, • homodyne Michelson • interferometer readout

  14. LISA InterferometryTeV II MeetingMadison, WiAugust 30th, 2006 Guido Mueller University of Florida mueller@phys.ufl.edu

  15. LISA Interferometry • Goal: • Measure distances with • 10 pm/rtHz accuracy • Basics: • Laser: • Wavelength: 1mm • Power: 1 W • Telescopes: • f/1 - Cassegrain • Diameter: 40cm •  Received power: ~100pW

  16. The Orbit Problem • Arm lengths change • by about 50.000km • during 12mts orbit • or ~1m/s. • Doppler shifts (~ MHz) • Unequal arm lengths • (frequency noise) • Telescope repointing (pointing noise) Very dynamic interferometer!

  17. dynamic range ~109 @ 5 mHz Requirement Phasemeter • Requirements: • 2-20 MHz signal frequencies, changing by several MHz • Frequency noise of 30Hz/Hz1/2 @ 1mHz • = 30000 cycl./Hz1/2 @ 1mHz • need to be resolved with 10-5 cycles/Hz1/2 accuracy! • Dynamic Range of 9 orders of magnitude. Solution: Tracking Filter JPL-Results

  18. Laser Frequency (Pre-) Stabilization Requirements: Frequency noise of 30Hz/Hz1/2 @ 1mHz (for Phase meter)

  19. Laser Frequency Stabilization II Arm locking: Different potential realizations Single Common Sagnac Round-trip arm length Difference between arms Sagnac effect (rotation)

  20. Latest TabletopResults of Arm locking Still a couple flaws in the experiment. But progressing well

  21. Key components perform and work at or below LISA requirements Arm Locking: will reduce requirements on other subsystems Not yet demonstrated at the final level (getting close) Main issues left for Interferometry: Stability of Materials and Components Actuators … standard stuff LISA INTERFEROMETRY TAKE AWAY

  22. Will detect the big stuff: SMBH mergers 10000s galactic binaries (guaranteed) Extreme mass ratio inspirals Challenges: Data analysis: Extract all the signals GRS: How to create a freely falling mass? LTP: European Test mission in 2009 Interferometry: The main challenges are nearly solved Start to focus on components, bits, and pieces LISA Summary LISA Launch: 2015 (on NASA time scales)

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