1 / 11

LIGO: Laser Interferometer Gravitational-wave Observatory

3. 0. 3. (. ±. 0. 1. k. 0. m. m. s. ). LIGO: Laser Interferometer Gravitational-wave Observatory. 4 km & 2 km. WA. MIT. Caltech. Managed and operated by Caltech & MIT with funding from NSF Ground breaking 1995 1st interferometer lock 2000

joshwa
Download Presentation

LIGO: Laser Interferometer Gravitational-wave Observatory

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. 3 0 3 ( ± 0 1 k 0 m m s ) LIGO: Laser Interferometer Gravitational-wave Observatory 4 km & 2 km WA MIT Caltech • Managed and operated by Caltech & MIT with funding from NSF • Ground breaking 1995 • 1st interferometer lock 2000 • LIGO Scientific collaboration: 45 institutions, world-wide LA 4 km March 2, 2007 R Frey

  2. General Relativity • Some predictions: • Gravity influences both mass and energy • e.g. bending of light in regions with gravitational field • 1919 Eddington; Gravitational lensing: Einstein Cross • Many small deviations from Newtonian gravity in “weak” fields • Gravitational “redshift” (e.g. clocks on satellites are faster) • Perihelion advance of mercury • Global Positioning System would not work without GR corrections • “Strong” field effects • Black holes; Rs = 2GM/c2 • Spacetime structure of universe – evolution of spacetime from Big Bang • the “big stretch” • And gravitational radiation (gravitational waves) March 2, 2007 R Frey

  3. GWs in GR March 2, 2007 R Frey

  4. Required Gravitational Wave Sensitivity • GW emission requires time varying quadrupole moment of mass distribution • Strain estimate (h = L/ L): March 2, 2007 R Frey

  5. GW Interferometer Principle GW strain: h = L/ L March 2, 2007 R Frey

  6. S5 Science Run: LIGO at Design Sensitivity March 2, 2007 R Frey

  7. Science runs and sensitivity March 2, 2007 R Frey

  8. Coalescing Compact Binaries NS-NS, BH-BH, (BH-NS) binary systems Matched filter Template-less Matched filter March 2, 2007 R Frey

  9. Gravitational Radiation and Gamma-ray Bursts BATSE • Long-duration GRBs • Stronger afterglows → z • SNe or “hypernovae” • mean z  2.5 GSFC • Short-duration GRBs • Until 2005, no measured z’s → enter Swift • Now: a few z’s → “compact binary mergers” GRB030329 HETE-2 • mergers are efficient GW radiators • much smaller z’s (mean  0.4) Oct 6, 2005 March 2, 2007 R Frey

  10. 2006 2007 2008 2009 2010 2011 2012 2013 2014 The Future: Enhanced and Advanced LIGO Enhanced LIGO (S6) • readout noise; laser power • Commission AdLIGO readout with real IFOs • reduce AdLIGO startup time Advanced LIGO • Major upgrades: optics, lasers, suspensions, ... • 10 better sensitivity S5 Run S7 S6 LIGO enhanced LIGO AdvancedLIGO News flash: Advanced LIGO is in the FY08 President’s budget build hardware installation science March 2, 2007 R Frey

  11. Advanced LIGO reach (example) NS-NS inspiral search NS-NS sources (h sensitivity)2.7 h sensitivity will improve by 10, with improved bandwidth March 2, 2007 R Frey

More Related