1 / 26

LISA and Beyond

LISA and Beyond. Neil Cornish Louis 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. Courtesy Rutherford Appelton Lab.

JasminFlorian
Télécharger la présentation

LISA and Beyond

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

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

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

  12. AM - FM - Stereo Channel 2 Channel 1

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

  14. The LISA Simulator

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

  16. 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)

  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 Amplitude modulation Doppler modulation Monochromatic Binaries. Fixed SNR=10

  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

More Related