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Searching for gravitational waves with lasers (LIGO)

Searching for gravitational waves with lasers (LIGO). Rick Savage Caltech LIGO Hanford Observatory - Richland, WA. Black holes and time warps. Transferred to UCLA in Physics in 1974 Jan 1975 S tarted working for F. Chen and N. Luhmann as undergraduate lab assistant (with Doug Cook)

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Searching for gravitational waves with lasers (LIGO)

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  1. Searching for gravitational waves with lasers (LIGO) Rick Savage CaltechLIGO Hanford Observatory - Richland, WA

  2. Black holes and time warps • Transferred to UCLA in Physics in 1974 • Jan 1975 • Started working for F. Chen and N. Luhmann as undergraduate lab assistant (with Doug Cook) • Alain Semet, John Turcek, Steve Obenschain, Jim Holt, Mark Herbst, et al. • 1976-1986 Plasma diagnostics • N. Luhmann, T. Peebles, H. Fetterman, et al. • Microtorr, macrotorr, UT FRC, FIR lasers, CO2 lasers • 1986 – 1992 Laser / Plasma interactions • Graduate school in EE at UCLA – Chan Joshi • Masters thesis – Degenerate four-wave mixing in heated CO2gas • PhD thesis – Frequency upshiftingof electromagnetic radiation via an underdense relativistic ionization front • 1992 – present • LIGO project – Caltech until 1997 then LIGO Hanford Observatory in Richland, WA UCLA Symposium F2C@80 Nov. 2009

  3. http://www.einsteinsmessengers.org/ UCLA Symposium F2C@80 Nov. 2009

  4. LIGO: Laser Interferometer Gravitational-wave Observatory Hanford, WA MIT 3002 km (L/c = 10 ms) Caltech • Managed and operated by Caltech & MIT with funding from NSF • Goal: Direct observation ofgravitational waves • Open an new observationalwindow on the Universe Livingston, LA

  5. LIGO Scientific Collaboration LIGO Scientific Collaboration • University of Michigan • University of Minnesota • The University of Mississippi • Massachusetts Inst. of Technology • Monash University • Montana State University • Moscow State University • National Astronomical Observatory of Japan • Northwestern University • University of Oregon • Pennsylvania State University • Rochester Inst. of Technology • Rutherford Appleton Lab • University of Rochester • San Jose State University • Univ. of Sannio at Benevento, and Univ. of Salerno • University of Sheffield • University of Southampton • Southeastern Louisiana Univ. • Southern Univ. and A&M College • Stanford University • University of Strathclyde • Syracuse University • Univ. of Texas at Austin • Univ. of Texas at Brownsville • Trinity University • Tsinghua University • Universitat de les IllesBalears • Univ. of Massachusetts Amherst • University of Western Australia • Univ. of Wisconsin-Milwaukee • Washington State University • University of Washington • Australian Consortiumfor InterferometricGravitational Astronomy • The Univ. of Adelaide • Andrews University • The Australian National Univ. • The University of Birmingham • California Inst. of Technology • Cardiff University • Carleton College • Charles Sturt Univ. • Columbia University • CSU Fullerton • Embry Riddle Aeronautical Univ. • EötvösLoránd University • University of Florida • German/British Collaboration forthe Detection of Gravitational Waves • University of Glasgow • Goddard Space Flight Center • Leibniz Universität Hannover • Hobart & William Smith Colleges • Inst. of Applied Physics of the Russian Academy of Sciences • Polish Academy of Sciences • India Inter-University Centrefor Astronomy and Astrophysics • Louisiana State University • Louisiana Tech University • Loyola University New Orleans • University of Maryland • Max Planck Institute for Gravitational Physics UCLA Symposium F2C@80 Nov. 2009

  6. General relativity – gravitational waves “Matter tells spacetime how to curve.Spacetime tell matter how to move.”J. A Wheeler Albert Einstein1916 GW: oscillating quadrupolar strain in spacetime Laser Interferometer UCLA Symposium F2C@80 Nov. 2009

  7. Detection of graviational waves Michelson interferometer - differential lengthchange sensor UCLA Symposium F2C@80 Nov. 2009

  8. Do they exist? Indirect evidence Pulsar System PSR 1913 + 16 (R.A. Hulse, J.H. Taylor Jr, 1975) Orbit will continue to decay over the next ~300 million years, until coalescence Gravitational wave emission will be strongest near the end (Weisberg, Taylor) UCLA Symposium F2C@80 Nov. 2009

  9. Capturing the waveform Sketch: Kip Thorne UCLA Symposium F2C@80 Nov. 2009

  10. Sources • Coalescing Binary Systems • Neutron stars, low mass black holes, and NS/BS systems ‘Bursts’ galactic asymmetric core collapse supernovae cosmic strings ??? Credit: AEI, CCT, LSU Credit: Chandra X-ray Observatory Cosmic GW background stochastic,incoherent background Continuous Sources Spinning neutron stars probe crustal deformations UCLA Symposium F2C@80 Nov. 2009 Casey Reed, Penn State NASA/WMAP Science Team

  11. Ligo detectors Power Recycled Michelson Interferometer with Fabry-Perot Arm Cavities 4 km-longFabry-Perotarm cavity recycling mirror test masses Laser beam splitter signal UCLA Symposium F2C@80 Nov. 2009

  12. iLigo hardware UCLA Symposium F2C@80 Nov. 2009

  13. S5 Science Run Nov 2005 – Oct 2007 UCLA Symposium F2C@80 Nov. 2009

  14. Scientific results of S5 run • No detections (so far) - data still being analyzed • Astrophysical results – upper limits“If LIGO didn’t detect it, then it can’t be bigger than …” • CRAB pulsar – “no more than 4 percent of the energy loss of the pulsar is caused by the emission of gravitational waves.”(ApJL 683, L45) • Gamma ray burst GRB 070201 – LIGO “results give an independent wayto reject hypothesis of a compact binaryprogenitor in M31”(ApJ 2008, 681, 1419) • Upper limit on the stochastic gravitational wave background(http://www.nature.com/nature/journal/v460/n7258/pdf/nature08278.pdf) Credits for X-ray Image: NASA/CXC/ASU/J. Hester et al. Credits for Optical Image: NASA/HST/ASU/J. Hester et al. UCLA Symposium F2C@80 Nov. 2009

  15. UCLA Symposium F2C@80 Nov. 2009

  16. Enhanced LIGO LIGO today 108 ly Adv. LIGO Credit: R.Powell, B.Berger UCLA Symposium F2C@80 Nov. 2009

  17. UCLA Symposium F2C@80 Nov. 2009

  18. 10 W to 200 W laser source UCLA Symposium F2C@80 Nov. 2009

  19. Single to quadruple pendulum UCLA Symposium F2C@80 Nov. 2009

  20. Passive to active vibration isolation UCLA Symposium F2C@80 Nov. 2009

  21. Time warps UCLA Laser/Plasma interactions UCLA Symposium F2C@80 Nov. 2009

  22. UCLA Symposium F2C@80 Nov. 2009

  23. LIGO Scientific Collaboration UCLA Symposium F2C@80 Nov. 2009

  24. HANFORD Washington MIT Boston 3 0 3 ( 0 ± 1 k 0 m m s ) CALTECH Pasadena LIVINGSTON Louisiana Laser Interferometer Gravitational-wave Observatory • Started as a collaboration between Caltech and MIT • Goal: direct observation of gravitational waves • Open a new observational window on the Universe UCLA Symposium F2C@80 Nov. 2009

  25. LIGO Hanford Observatory • South-central Washington • Where Columbia, Yakima, and Snake rivers converge UCLA Symposium F2C@80 Nov. 2009

  26. Frank’s thinking ….. inflatable kiyak ? …. LIGO Doug CookColumbia River credit: Google Maps UCLA Symposium F2C@80 Nov. 2009

  27. UCLA Symposium F2C@80 Nov. 2009

  28. UCLA Symposium F2C@80 Nov. 2009

  29. closer look – more lasers and optics UCLA Symposium F2C@80 Nov. 2009

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