1 / 29

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)

trinh
Télécharger la présentation

Searching for gravitational waves with lasers (LIGO)

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. 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

More Related