1. 08/31/2006 ~ 2015 3 Mission specific challenges: Data Analysis GRS Interferometry

2. 08/31/2006

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

5. 08/31/2006

6. Generate realistic data streams for data analysis tests

7. 08/31/2006 Data Analysis Challenge: Can we identify all signals ?

8. 08/31/2006 Data Analysis: Galactic Binary Routines

9. 08/31/2006

10. Data Analysis Take Away 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

11. 08/31/2006 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

12. 08/31/2006 GRS Gravitational Reference Sensor (GRS) in the LISA Spacecraft

13. 08/31/2006 Baseline Design: Two Cubic Proof Masses per Spacecraft Proof Mass Proof Mass To and from Remote Spacecraft Waveplate Transmissive optics Sensitive path

14. 08/31/2006 LISA Test Package: ESA Space mission to test the GRS Launch: 2009! Performance Goal: Acceleration < 10 -14 m/s -2/3 (10 times LISA) Understand the system

15. 08/31/2006 LISA Noise Sources Additional leading term: Voltage Reference Instability

16. 08/31/2006 Alternative Single PM Design Outgoing Laser Beam Proof Mass Large gap GRS Housing Optical Readout Beam Telescope Incoming Laser Beam Details Shown in Figure 2 Sun, Allen, Buchman, DeBra, Byer, CQG (22) 2005 S287-S296

17. 08/31/2006 LISA Test Package: ESA Space mission to test the GRS Launch: 2009 Two inertial sensors, homodyne Michelson interferometer readout GRS Take away:

18. 08/31/2006 LISA Interferometry TeV II Meeting Madison, Wi August 30 th, 2006 mueller@phys.ufl.edu Guido Mueller University of Florida

19. 08/31/2006 LISA Interferometry Goal: Measure distances with 10 pm/rtHz accuracy Basics: Laser: Wavelength: 1  m Power: 1 W Telescopes: f/1 - Cassegrain Diameter: 40cm  Received power: ~100pW

20. 08/31/2006 Arm lengths change by about 50.000 km during 12 mts orbit or ~1 m/s.  Doppler shifts (~ MHz)  Unequal arm lengths (frequency noise)  Telescope repointing (pointing noise) The Orbit Problem Very dynamic interferometer!

21. 08/31/2006 Requirements: 2-20 MHz signal frequencies, changing by several MHz Frequency noise of 30Hz/Hz 1/2 @ 1mHz = 30000 cycl./Hz 1/2 @ 1mHz need to be resolved with 10 -5 cycles/Hz 1/2 accuracy!  Dynamic Range of 9 orders of magnitude. Solution: Tracking Filter Phasemeter dynamic range ~10 9 @ 5 mHz Requirement JPL-Results

22. 08/31/2006 Laser Frequency (Pre-) Stabilization Requirements: Frequency noise of 30Hz/Hz 1/2 @ 1mHz (for Phase meter)

23. 08/31/2006 SingleCommon Sagnac Round-trip arm lengthDifference between armsSagnac effect (rotation) Arm locking: Different potential realizations Laser Frequency Stabilization II

24. 08/31/2006 Latest Tabletop Results of Arm locking Still a couple flaws in the experiment. But progressing well

25. 08/31/2006 LISA INTERFEROMETRY TAKE AWAY 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

26. 08/31/2006 LISA Summary 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 Launch: 2015 (on NASA time scales)