LISA and Beyond

Neil CornishLouis Rubbo, Seth Timpano & Jeff Crowder

Outline

• LISA (Laser Interferometer Space Antenna)

• LIASE (Laser Interferometer Arc-Second Explorer)

• BBO (Big Bang Observatory)

Laser Interferometer Space Antenna

QuickTime™ and aCinepak decompressorare needed to see this picture.

Courtesy Rutherford Appelton Lab

LISA compliments LIGO

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

LISA Astronomy

Kip Thorne

SMBH Inspiral at z =1

€

106M8 −106M8

SMBH Inspiral at z = 1

€

106M8 −106M8

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:

• 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)

Galactic Background and Confusion Noise

Main noise source for LISA is signal!

Timpano, Rubbo & Cornish

AM - FM - Stereo

QuickTime™ and aGIF decompressorare needed to see this picture.

Channel 1

Channel 2

N. J. Cornish and L. J. Rubbo, Phys. Rev. D 67, 022001 (2003)

ˆnSun

Earth

LISA

GW Source

http:/www.physics.montana.edu/LISA

Forward Modeling

The LISA Simulator

Galactic Background

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

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)

The Future is in GEMSGravitational-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?

LISA Angular Resolution

Monochromatic Binaries. Fixed SNR=10

Doppler modulationAmplitude 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

ConclusionsMany 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 5x10^9 m 3x10^-15

LIASE 1.0 m 50 W 5x10^7 m 3x10^-16

BBO 3.5 m 300 W 5x10^7 m 3x10^-17