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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
QuickTime™ and a Cinepak decompressor are 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
6
6
10
M
10
M
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SMBH Inspiral at z = 1
6
6
10
M
10
M

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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
QuickTime™ and a GIF decompressor are needed to see this pi cture.
Channel 2
Channel 1
Forward Modeling
LISA
GW Source
Earth
Sun
n̂
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-ElectroMagnetic Sources
•
Break Degeneracies
•
•
: EM
(Spc. Binaries)
Cover Gaps
•
•
•
GW
GW : EM
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
1W
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