Overview Ground-based Interferometers. Barry Barish Caltech Amaldi-6 20-June-05
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1 Overview Ground-based Interferometers Barry Barish Caltech Amaldi-6 20-June-05
2 TAMA Japan 300m Interferometer Detectors LIGO Louisiana 4000m Virgo Italy 3000m AIGO Australia future GEO Germany 600m LIGO Washington 2000m & 4000m 20-June-05 Amaldi-6 - Interferometer Overview - Barish 2
3 Network of Interferometers LIGO GEO Virgo TAMA decompose detection locate the the confidence polarization sources of gravitational waves AIGO 20-June-05 Amaldi-6 - Interferometer Overview - Barish 3
4 Interferometer Concept causing the interference pattern to change at the photodiode As a wave passes, Suspended the arm Masses lengths change in different ways. 20-June-05 Amaldi-6 - Interferometer Overview - Barish 4
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 20-June-05 Amaldi-6 - Interferometer Overview - Barish 5
6 TAMA June-05 Amaldi-6 - Interferometer Overview - Barish 6
7 Automated Data Taking in DT9 - 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 Self-switching sub-system Logic circuit + Embedded micro processor Laser source control MC control Laser intensity stabilization Beam axes control 20-June-05 Amaldi-6 - Interferometer Overview - Barish 7
8 Sensitivity in DT9 Recycling gain: 4.5 Extended control band width for the laser frequency Improved strain sensitivity: h=1.7x10-21 /Hz 20-June-05 Amaldi-6 - Interferometer Overview - Barish 8
9 TAMA Observable distance for NS inspiral binaries 20-June-05 Amaldi-6 - Interferometer Overview - Barish 9
10 TAMA Ringdown Analysis 20-June-05 Amaldi-6 - Interferometer Overview - Barish 10
11 GEO600
12 GEO 600 Optical Layout 20-June-05 Amaldi-6 - Interferometer Overview - Barish 12
13 GEO Sensitivity Evolution 20-June-05 Amaldi-6 - Interferometer Overview - Barish 13
14 LIGO LIGO Hanford LIGO Livingston 20-June-05 Amaldi-6 - Interferometer Overview - Barish 14
15 Evolution of LIGO Sensitivity 20-June-05 Amaldi-6 - Interferometer Overview - Barish 15
16 Active Seismic Isolation at LLO Hydraulic external preisolator (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 20-June-05 Amaldi-6 - Interferometer Overview - Barish 16
17 Active Seismic Isolation at LLO Can lock (and do commissioning work!) during daytime Able to stay locked even when train passes nearby 20-June-05 Amaldi-6 - Interferometer Overview - Barish 17
18 LIGO Livingston Sensitivity 20-June-05 Amaldi-6 - Interferometer Overview - Barish 18
19 LIGO S4 Best Performance 20-June-05 Amaldi-6 - Interferometer Overview - Barish 19
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. 20-June-05 Amaldi-6 - Interferometer Overview - Barish 20
21 LIGO GEO Directed Pulsar Search 28 Radio Sources 20-June-05 Amaldi-6 - Interferometer Overview - Barish 21
22 GEO-LIGO - Results h 0 95% UL Pulsars ellipticity ε Pulsars < h 0 < < h 0 < h 0 > < ε < < ε < ε > Lowest 95% UL on h 0 = (J D) Crab pulsar Lowest bound on e = (J ) Crab pulsar: h 0 = ε = (~30 times spin-down upper limit) 20-June-05 Amaldi-6 - Interferometer Overview - Barish 22
23 Detection of Periodic Sources Pulsars in our galaxy 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. NEW RESULT 28 known pulsars NO gravitational waves ε < (no mountains > 10 cm ALL SKY SEARCH enormous computing challenge 20-June-05 Amaldi-6 - Interferometer Overview - Barish 23
24 LIGO Pulsar Search using home pc s BRUCE ALLEN Project Leader Univ of Wisconsin Milwaukee LIGO, UWM, AEI, APS 20-June-05 Amaldi-6 - Interferometer Overview - Barish 24
25 Virgo 20-June-05 Amaldi-6 - Interferometer Overview - Barish 25
26 Virgo Seismic Performance Thermal noise 20-June-05 Amaldi-6 - Interferometer Overview - Barish 26
27 Virgo - Sensitivity Goal Designed to have good sensitivity at low frequencies 20-June-05 Amaldi-6 - Interferometer Overview - Barish 27
28 Virgo Commissioning Extragalactic sensitivity to NS/NS coalescences 55 kpc 20-June-05 Amaldi-6 - Interferometer Overview - Barish 28
29 Advanced LIGO Active Seismic Multiple Suspensions Improved Optics Higher Power Laser 20-June-05 Amaldi-6 - Interferometer Overview - Barish 29
30 Advanced LIGO Enhanced Systems laser suspension seismic isolation test mass Rate Improvement ~ narrow band optical configuration 20-June-05 Amaldi-6 - Interferometer Overview - Barish 30
31 From Amaldi-6 Onwards From Present Generation Advanced Detectors Next Generation Detectors (QND) From 8 Mpc (NN inspiral) 200 Mpc and beyond From Upper Limits Searches Detections From Generic Waveforms Specified Waveforms From Single Detectors Global Networks 20-June-05 Amaldi-6 - Interferometer Overview - Barish 31
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