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Cutting-edge Interferometer Technology: Amaldi-6 Overview with Barry Barish

Learn about the groundbreaking Amaldi-6 Interferometer network, including LIGO, Virgo, and more, pioneering the detection and localization of gravitational wave sources. Delve into the technical details of the interferometer concept, noise limitations, automated data-taking systems, and advanced sensitivity achievements. Explore the active seismic isolation capabilities at LIGO Livingston, advancements in detecting periodic sources like pulsars, and the collaborative efforts in searching for and analyzing gravitational wave signals. Discover the latest developments from Amaldi-6 and beyond, aiming to push the sensitivity boundaries for the next generation of interferometers.

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Cutting-edge Interferometer Technology: Amaldi-6 Overview with Barry Barish

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  1. Overview Ground-based Interferometers Barry Barish Caltech Amaldi-6 20-June-05

  2. LIGO Louisiana 4000m Interferometer Detectors TAMA Japan 300m Virgo Italy 3000m GEO Germany 600m AIGO Australia future LIGO Washington 2000m & 4000m Amaldi-6 - Interferometer Overview - Barish

  3. Network of Interferometers LIGO Virgo GEO TAMA AIGO decompose the polarization of gravitational waves detection confidence locate the sources Amaldi-6 - Interferometer Overview - Barish

  4. As a wave passes, the arm lengths change in different ways…. Interferometer Concept …causing the interference pattern to change at the photodiode Suspended Masses Amaldi-6 - Interferometer Overview - Barish

  5. Limiting Noise Sources • Seismic noise & vibration limit at low frequencies • Atomic vibrations (Thermal Noise) inside components limit at mid frequencies • Quantum nature of light (Shot Noise) limits at high frequencies • Myriad details of the lasers, electronics, etc., can make problems above these levels Amaldi-6 - Interferometer Overview - Barish

  6. TAMA 300 Amaldi-6 - Interferometer Overview - Barish

  7. Automated Data Taking in DT9 - Self-switching sub-system Logic circuit + Embedded micro processor Laser source control MC control Laser intensity stabilization Beam axes control Master-system (intelligent switching) PC + PCI boards + LabVIEW 64ch digital I/O 16ch A/D + 24ch D/A Lock acquisition Auto adjustment Interface with external system Amaldi-6 - Interferometer Overview - Barish

  8. Sensitivity in DT9 Recycling gain: 4.5 Extended control band width for the laser frequency Improved strain sensitivity: h=1.7x10-21 /Hz1/2 @1kHz Amaldi-6 - Interferometer Overview - Barish

  9. Observable distance for NS inspiral binaries TAMA Amaldi-6 - Interferometer Overview - Barish

  10. TAMA Ringdown Analysis Amaldi-6 - Interferometer Overview - Barish

  11. GEO600

  12. GEO 600 – Optical Layout Amaldi-6 - Interferometer Overview - Barish

  13. GEO Sensitivity Evolution Amaldi-6 - Interferometer Overview - Barish

  14. LIGO LIGO Hanford LIGO Livingston Amaldi-6 - Interferometer Overview - Barish

  15. Evolution of LIGO Sensitivity Amaldi-6 - Interferometer Overview - Barish

  16. Active Seismic Isolation at LLO • Hydraulic external pre-isolator (HEPI) • Signals from sensors on ground and cross-beam are blended and fed into hydraulic actuators • Status: • Installed on all 4 piers at each of nine vacuum chambers • System is operational Amaldi-6 - Interferometer Overview - Barish

  17. Active Seismic Isolation at LLO • Can lock (and do commissioning work!) during daytime • Able to stay locked even when train passes nearby Amaldi-6 - Interferometer Overview - Barish

  18. LIGO Livingston Sensitivity Amaldi-6 - Interferometer Overview - Barish

  19. LIGO S4 – Best Performance Amaldi-6 - Interferometer Overview - Barish

  20. Detection of Periodic Sources • Pulsars in our galaxy:“periodic” • search for observed neutron stars • all sky search (computing challenge) • r-modes • Frequency modulation of signal due to Earth’s motion relative to the Solar System Barycenter, intrinsic frequency changes. • Amplitude modulation due to the detector’s antenna pattern. Amaldi-6 - Interferometer Overview - Barish

  21. LIGO – GEO Directed Pulsar Search 28 Radio Sources Amaldi-6 - Interferometer Overview - Barish

  22. GEO-LIGO - Results • Lowest 95% UL on h0 = 1.7 10-24 (J1910-5959D) • Lowest bound on e = 4.5 10-6 (J2124-3358) • Crab pulsar: • h0 = 4.1 10-23 • e = 2.1 10-2 (~30 times spin-down upper limit) Crab pulsar Amaldi-6 - Interferometer Overview - Barish

  23. Detection of Periodic Sources • Frequency modulationof signal due to Earth’s motion relative to the Solar System Barycenter, intrinsic frequency changes. • Pulsars in our galaxy NEW RESULT 28 known pulsars NO gravitational waves e < 10-5 – 10-6 (no mountains > 10 cm • Amplitude modulationdue to the detector’s antenna pattern. ALL SKY SEARCH enormous computing challenge Amaldi-6 - Interferometer Overview - Barish

  24. Einstein@Home LIGO Pulsar Search using home pc’s BRUCE ALLEN Project Leader Univ of Wisconsin Milwaukee LIGO, UWM, AEI, APS http://einstein.phys.uwm.edu Amaldi-6 - Interferometer Overview - Barish

  25. Virgo Amaldi-6 - Interferometer Overview - Barish

  26. Thermal noise Virgo Seismic Performance Amaldi-6 - Interferometer Overview - Barish

  27. Virgo - Sensitivity Goal Designed to have good sensitivity at low frequencies Amaldi-6 - Interferometer Overview - Barish

  28. Extragalactic sensitivity to NS/NS coalescences 55 kpc Virgo Commissioning Amaldi-6 - Interferometer Overview - Barish

  29. Advanced LIGO Multiple Suspensions Active Seismic Improved Optics Higher Power Laser Amaldi-6 - Interferometer Overview - Barish

  30. Advanced LIGO • Enhanced Systems • laser • suspension • seismic isolation • test mass Rate Improvement~ 104 + narrow band optical configuration Amaldi-6 - Interferometer Overview - Barish

  31. From Amaldi-6 Onwards • From Present GenerationAdvanced Detectors Next Generation Detectors (QND) • From 8 Mpc (NN inspiral)200 Mpc and beyond • From Upper LimitsSearches Detections • From Generic WaveformsSpecified Waveforms • From Single DetectorsGlobal Networks Amaldi-6 - Interferometer Overview - Barish

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