1. LISA and Beyond Neil Cornish Louis Rubbo, Seth Timpano & Jeff Crowder

2. Outline LISA (Laser Interferometer Space Antenna) LIASE (Laser Interferometer Arc-Second Explorer) BBO (Big Bang Observatory)

3. Laser Interferometer Space Antenna Courtesy Rutherford Appelton Lab

4. LISA compliments LIGO

5. LISA = LIGO in Space /  Synthetic vs. Fabrey-Perot Interferometery  Wavelengths comparable to size of detector  Free running vs. locked (Hetrodyne detection) Key Technologies  Accelerometers (disturbance reduction system)  Ultra stable lasers and clocks

6. LISA Astronomy Kip Thorne

7. SMBH Inspiral at z =1

9. LISA Science  Detect every SMBH & IMBH binary merger in the Universe  Resolve ~ 3000 stellar binaries in Galaxy  Holiodesy/Bothrodesy  Graviton Mass  M-Theory CGB  Cosmic Strings

10. Data Analysis: Simple Waveforms High Signal/Noise (Too) Many sources Complex modulation One detector Complex Waveforms Poor Signal/Noise (Too) Few sources Weak modulation Two detectors LISA LIGO (Exceptions: EMR, SMBH Mergers) (Exception: Isolated Pulsars)

11. Galactic Background and Confusion Noise Main noise source for LISA is signal! Timpano, Rubbo & Cornish

12. AM - FM - Stereo Channel 1 Channel 2

13. N. J. Cornish and L. J. Rubbo, Phys. Rev. D 67, 022001 (2003) Sun Earth LISA GW Source http:/www.physics.montana.edu/LISA Forward Modeling

14. The LISA Simulator

15. Galactic Background Timpano, Rubbo & Cornish. (Similar work by Benacquista)

16. Astrophysical Information Encoded in Time Series Internal Parameters External Parameters Time series depends on many source parameters Can estimate parameter resolution using Fisher Information Matrix (Cutler, Hellings & Moore, Vecchio, Seto, Hughes) Many parameters highly correlated (Cutler) Many sources that interfere (Cornish & Crowder) Coming soon: The LISA Calculator (Java web tool)

17. The Future is in GEMS Gravitational-ElectroMagnetic Sources Break Degeneracies GW : EM (Spc. Binaries) Cover Gaps GW : EM (SMBHB) GW : EM (LMXBs) Verify Source Identity Can we identify optical counterparts to LISA sources?

18. LISA Angular Resolution Monochromatic Binaries. Fixed SNR=10 Doppler modulationAmplitude modulation

19. LISA Angular Resolution Z=1, Final Year

20. Laser Interferometer Arc Second Explorer

21. LIASE Angular Resolution z=1, Final Year

22. Big Bang Observatory P.I. Phinney. Co.I’s Bender, Buchman, Cornish, Fritschel, Folkner, Merkowitz.

23. Big Bang Observatory

24. Cosmological Gravitational Wave Background = BBO

25. BBO Angular Resolution (For foreground Subtraction) Z=1, Final Year

26. Conclusions Many science drivers will shape future detectors. In almost every case improved angular resolution and electromagnetic counterparts will be very valuable. Amazing things are possible for large sums of money MirrorLaserArmsAccl. LISA0.3 m1 W5x10^9 m3x10^-15 LIASE1.0 m50 W5x10^7 m3x10^-16 BBO3.5 m300 W5x10^7 m3x10^-17