2. Searching for gravitational waves with LIGO An introduction to LIGO and a few things gravity wave Dr. Michael Landry LIGO Hanford Observatory California Institute of Technology

3. 2 LIGO in 30 seconds 2. Gravitational Waves: Never before directly detected 1. Gravitational Waves: Not EM or particles

4. 3 Gravitational wave astronomy in 30 seconds

5. 4 Talk overview Sources »What are gravitational waves? »Why look for them? »Sources: what makes them? Observatories »LIGO. Networks. Interferometers »Overview of a Michelson interferometer »Some LIGO installations »Strain curves and Science mode running Briefly! Einstein@home: a search for continuous gravitational waves

6. 5 Gravity: the Old School Sir Isaac Newton, who invented the theory of gravity and all the math needed to understand it

7. 6 Newton’s theory: good, but not perfect! Mercury’s orbit precesses around the sun-each year the perihelion shifts 560 arcseconds per century But this is 43 arcseconds per century too much! (discovered 1859) This is how fast the second hand on a clock would move if one day lasted 4.3 billion years! Mercury Sun perihelion Image from Jose Wudka Urbain Le Verrier, discoverer of Mercury’s perihelion shift anomaly Image from St. Andrew’s College

8. 7 Einstein’s Answer: General Relativity  Space and time (spacetime) are curved.  Matter causes this curvature  Space tells matter how to move  This looks to us like gravity Picture from Northwestern U.

9. 8 Space is curved. Really. Not only the path of matter, but even the path of light is affected by gravity from massive objects Einstein Cross Photo credit: NASA and ESA A massive object shifts apparent position of a star

10. 9 Important Signature of Gravitational Waves Gravitational waves shrink space along one axis perpendicular to the wave direction as they stretch space along another axis perpendicular both to the shrink axis and to the wave direction.

11. 10 What’s left behind when a star dies? Stars live… Stars die… And sometimes they leave behind exotic corpses… Supernova Ordinary star Black holes (credit : NASA/CXC/A. Hobart) Neutron stars, pulsars (credit : W. Feimer/STSI)

12. 11 Compact binary inspiral: “chirps” »NS-NS waveforms are well described »BH-BH need better waveforms Supernovae / GRBs: “bursts” »burst signals in coincidence with signals in electromagnetic radiation / neutrinos »all-sky untriggered searches too Cosmological Signal: “stochastic background” Pulsars in our galaxy: “periodic” »search for observed neutron stars »all-sky search (computing challenge) What might make Gravitational Waves?

13. 12 Supernova: Death of a Massive Star Spacequake should preceed optical display by ½ day Leaves behind compact stellar core, e.g., neutron star, black hole Strength of waves depends on asymmetry in collapse Observed neutron star motions indicate some asymmetry present Simulations do not succeed from initiation to explosions Credit: Dana Berry, NASA

14. 13 Supernova: Death of a Massive Star Spacequake should preceed optical display by ½ day Leaves behind compact stellar core, e.g., neutron star, black hole Strength of waves depends on asymmetry in collapse Observed neutron star motions indicate some asymmetry present Simulations do not succeed from initiation to explosions Credit: Dana Berry, NASA

15. 14 Sounds of Compact Star Inspirals Neutron-star binary inspiral: Black-hole binary inspiral:

16. 15 Gravitational-Wave Emission May be the “Regulator” for Accreting Neutron Stars Neutron stars spin up when they accrete matter from a companion Observed neutron star spins “max out” at ~700 Hz Gravitational waves are suspected to balance angular momentum from accreting matter Credit: Dana Berry, NASA

17. 16 Gravitational-Wave Emission May be the “Regulator” for Accreting Neutron Stars Neutron stars spin up when they accrete matter from a companion Observed neutron star spins “max out” at ~700 Hz Gravitational waves are suspected to balance angular momentum from accreting matter Credit: Dana Berry, NASA

18. 17 Neutron Binary System – Hulse & Taylor PSR 1913 + 16 -- Timing of pulsars   17 / sec Neutron Binary System separated by ~2x10 6 km m 1 = 1.44m  ; m 2 = 1.39m  ;  = 0.617 Prediction from general relativity spiral in by 3 mm/orbit rate of change orbital period ~ 8 hr Emission of gravitational waves Orbital decay : strong indirect evidence

19. 18 Orbital decay : strong indirect evidence Neutron Binary System – Hulse & Taylor PSR 1913 + 16 -- Timing of pulsars   17 / sec Neutron Binary System separated by ~2x10 6 km m 1 = 1.44m  ; m 2 = 1.39m  ;  = 0.617 Prediction from general relativity spiral in by 3 mm/orbit rate of change orbital period ~ 8 hr Emission of gravitational waves See “Tests of General Relativity from Timing the Double Pulsar” Science Express, Sep 14 2006 The only double-pulsar system know, PSR J0737-3039A/B provides an update to this result. Orbital parameters of the double-pulsar system agree with those predicted by GR to 0.05%

20. 19 Laser Beam Splitter End Mirror Screen Viewing Sketch of a Michelson Interferometer

21. 20 Gravitational Wave Detection Suspended Interferometers »Suspended mirrors in “free-fall” »Michelson IFO is “natural” GW detector »Broad-band response (~50 Hz to few kHz) »Waveform information (e.g., chirp reconstruction) power recycling mirror Fabry-Perot cavity 4km g.w. output port LIGO design length sensitivity: 10 -18 m

22. 21 Sensing the Effect of a Gravitational Wave Laser signal Gravitational wave changes arm lengths and amount of light in signal Change in arm length is 10 -18 meters, or about 2/10,000,000,000,000,000 inches

23. 22 How Small is 10 -18 Meter? Wavelength of light, about 1 micron One meter, about 40 inches Human hair, about 100 microns LIGO sensitivity, 10 -18 meter Nuclear diameter, 10 -15 meter Atomic diameter, 10 -10 meter

24. 23 LIGO (Washington) (4km and 2km) LIGO (Louisiana) (4km) Funded by the National Science Foundation; operated by Caltech and MIT; the research focus for more than 670 LIGO Scientific Collaboration members worldwide. LIGO sites

25. 24 The LIGO Observatories Adapted from “The Blue Marble: Land Surface, Ocean Color and Sea Ice” at visibleearth.nasa.gov NASA Goddard Space Flight Center Image by Reto Stöckli (land surface, shallow water, clouds). Enhancements by Robert Simmon (ocean color, compositing, 3D globes, animation). Data and technical support: MODIS Land Group; MODIS Science Data Support Team; MODIS Atmosphere Group; MODIS Ocean Group Additional data: USGS EROS Data Center (topography); USGS Terrestrial Remote Sensing Flagstaff Field Center (Antarctica); Defense Meteorological Satellite Program (city lights). LIGO Hanford Observatory (LHO) H1 : 4 km arms H2 : 2 km arms LIGO Livingston Observatory (LLO) L1 : 4 km arms 10 ms

26. 25 An International Network of Interferometers LIGO Simultaneously detect signal (within msec) detection confidence locate the sources decompose the polarization of gravitational waves GEO Virgo TAMA AIGO (proposed)

27. 26 Vacuum Chambers Provide Quiet Homes for Mirrors View inside Corner Station Standing at vertex beam splitter

28. 27 All-Solid-State Nd:YAG Laser Custom-built 10 W Nd:YAG Laser, joint development with Lightwave Electronics (now commercial product) Frequency reference cavity (inside oven) Cavity for defining beam geometry, joint development with Stanford

29. 28 Core Optics Suspension and Control Shadow sensors & voice-coil actuators provide damping and control forces Mirror is balanced on 30 micron diameter wire to 1/100 th degree of arc Optics suspended as simple pendulums

30. 29 Evacuated Beam Tubes Provide Clear Path for Light Vacuum required: <10 -9 Torr

31. 30 Evacuated Beam Tubes Provide Clear Path for Light Vacuum required: <10 -9 Torr Bakeout facts: 4 loops to return current, 1” gauge 1700 amps to reach temperature bake temp 140 degrees C for 30 days 400 thermocouples to ensure even heating each site has 4.8km of weld seams full vent of vacuum: ~ 1GJ of energy

32. 31 Seismic Isolation – Springs and Masses damped spring cross section

33. 32 LIGO detector facilities Seismic Isolation Multi-stage (mass & springs) optical table support gives 10 6 suppression Pendulum suspension gives additional 1 / f 2 suppression above ~1 Hz 10 2 10 0 10 -2 10 -4 10 -6 10 -8 10 -10 Horizontal Vertical 10 -6 Frequency (Hz) Transfer function

34. 33 Interferometer Length Control System Multiple Input / Multiple Output Three tightly coupled cavities Employs adaptive control system that evaluates plant evolution and reconfigures feedback paths and gains during lock acquisition (photodiode) 4km

35. 34 Calibrated output: LIGO noise history S1 S2 80kpc 1Mpc 15Mpc S1 S2 S3 S4 S5 Curves are calibrated interferometer output: spectral content of the gravity-wave channel

36. 35 The road to design sensitivity…

37. 36 Time line Inauguration 19992000200120022003 3 41 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 E2 Engineering E3 E5 E9E10 E7 E8 E11 First LockFull Lock all IFO 10 -17 10 -18 10 -20 10 -21 20042005 1 2 3 4 1 2 3 4 1 2 3 4 2006 First Science Data S1 S4 Science S2 Runs S3S5 10 -22 4K strain noiseat 150 Hz [Hz -1/2 ] Coincident science runs with GEO and TAMA 2007

38. 37 LIGO Hanford control room

39. 38 Einstein@home http://einstein.phys.uwm.edu/ Like SETI@home, but for LIGO/GEO data American Physical Society (APS) publicized as part of World Year of Physics (WYP) 2005 activities Use infrastructure/help from SETI@home developers for the distributed computing parts (BOINC) Goal: pulsar searches using ~1 million clients. Support for Windows, Mac OSX, Linux clients From our own clusters we can get ~ thousands of CPUs. From Einstein@home hope to get order(s) of magnitude more at low cost Great outreach and science education tool Currently : ~160,000 active users corresponding to about 85Tflops, about 200 new users/day

40. 39 What would a pulsar look like? Post-processing step: find points on the sky and in frequency that exceeded threshold in many of the sixty ten-hour segments Software-injected fake pulsar signal is recovered below Simulated (software) pulsar signal in S3 data

41. 40 Final S3 analysis results Data: 60 10-hour stretches of the best H1 data Post-processing step on centralized server: find points in sky and frequency that exceed threshold in many of the sixty ten-hour segments analyzed 50-1500 Hz band shows no evidence of strong pulsar signals in sensitive part of the sky, apart from the hardware and software injections. There is nothing “in our backyard”. Outliers are consistent with instrumental lines. All significant artifacts away from r.n=0 are ruled out by follow-up studies. WITH INJECTIONS WITHOUT INJECTIONS

42. 41 Summary remarks Initial LIGO achieved design sensitivity in Nov 05, a major milestone LIGO/GEO then launched the coincident S5 science run, which is to ran until Sep 30, 2007 Host of searches underway: analyses ongoing of S5 data – no detections yet! Enhanced LIGO upgrade 2007-2009, factor of ~2 in sensitivity improvement, mostly complete S6: underway Advanced LIGO upgrade underway: slated for ~2011 to dramatically improve sensitivity We should be detecting gravitational waves regularly within the next 10 years!

43. 42 LIGO - Virgo LIGO+ Virgo+ AdvLIGO AdvVirgo A hope for the near future: The Beginning of a New Astronomy…