LISA and Beyond Neil Cornish Louis Rubbo Seth

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

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

Laser Interferometer Space Antenna Courtesy Rutherford Appelton Lab

LISA compliments LIGO

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

LISA Astronomy Kip Thorne

SMBH Inspiral at z =1

SMBH Inspiral at z = 1

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

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

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

AM - FM - Stereo Channel 2 Channel 1

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

The LISA Simulator

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

Astrophysical Information Encoded in Time Series Time series depends on many source parameters Internal Parameters External 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)

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

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

LISA Angular Resolution Z=1, Final Year

Laser Interferometer Arc Second Explorer

LIASE Angular Resolution z=1, Final Year

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

Big Bang Observatory

Cosmological Gravitational Wave Background = BBO

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

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 Mirror Laser Arms Accl. LISA 0. 3 m 1 W 5 x 10^9 m 3 x 10^-15 LIASE 1. 0 m 50 W 5 x 10^7 m 3 x 10^-16 BBO 3. 5 m 300 W 5 x 10^7 m 3 x 10^-17