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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