Gravitationswellen. Wirkung auf Punktmassen. für astrophysikalische Quellen h ~ h L L
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1 G-Wellendetektoren
2 Gravitationswellen Wirkung auf Punktmassen h L L für astrophysikalische Quellen h ~
3 Chirp Signal We can use weak-field gravitational waves to study strong-field general relativity.
4 Joe WEBER und der Anfang
5 LSU Zylinder-Detektor
6
7
8 Prinzip eines Michelson Interferometers
9 LIGO Hanford, Washington Livingston, Lousiana
10 The LIGO Project LIGO: Laser Interferometer Gravitational-Wave Observatory Detection, followed by astronomy LIGO Science Collaboration (LSC) includes many institutions Funded by US National Science Foundation Max Planck Institute Andrews University Australian National Univ. Caltech Cardiff University Carleton College Charles Sturt Univ. Columbia University Embry-Riddle Aero. Univ. Eӧtvӧs University Hobart & William Smith Institute of Applied Physics, Nizhny Novgorod Inter-University Centre for Astronomy and Astrophysics, Pune Leibniz Universität Hannover LIGO Hanford Observatory LIGO Livingston Observatory Massachusetts Inst. of Technology Louisiana State Louisiana Tech McNeese State Univ. Montana State Univ. Moscow State Univ. NASA/Goddard Flight Ctr. Nat. Astronomical Observatory of Japan Northwestern University Rochester Inst. of Technology Rutherford Appleton Lab. San Jose State Univ. Sonoma State Univ. Southeastern Louisiana Southeastern Univ. Southern University Stanford University Syracuse University Penn State Univ. University of Melbourne Univ. of Mississippi Univ. of Sheffield Univ. of Texas at Austin Univ. of Texas at Brownsville Universitat de les Illes Balears Trinity University Univ. of Adelaide University of Birmingham Univ. of Florida Univ. of Glasgow University of Maryland Univ. of Mass. Amherst University of New Hampshire Univ. of Michigan Univ. of Minnesota University of Oregon Univ. of Rochester Univ. of Salerno Univ. of Southhampton Univ. of Sannio at Benevento University of Strathclyde University of Western Australia University of Wisconsin-Milwaukee Washington State University
11 The LIGO Observatories LIGO Hanford Observatory (LHO) (4km and 2km in same vacuum) LIGO Livingston Observatory (LLO)
12 Seismic Isolation Passive (to reduce noise in sensitive freq. band) Active (to improve lock acquisition/maintenance)
13 Suspended Test Masses Optics are 25 cm diameter, 10 cm thick, 10.7 kg, of high purity fused silica. They must have <50 ppm scattering losses, <1 ppm absorption losses. The optics are suspended to attenuate seismic motion above the pendulum frequency. f f 0
14 Seismic: Attenuated seismic noise h(f) 1/f 12 Suspension thermal: Viscously damped pendulum h(f) 1/f 2 Shot Noise: Photon Counting Statistics h(f) f
15 Seismic Internal thermal Shot noise and pole frequency LIGO-G SMU Physics Seminar, March 29,
16 LIGO Observatories Hanford, WA (H1 4km, H2 2km) - Interferometers are aligned to be as close to parallel to each other as possible - Observing signals in coincidence increases the detection confidence - Determine source location on the sky, propagation speed and polarization of the gravity wave Livingston, LA (L1 4km) LIGO GEO Virgo TAMA AIGO (proposed)
17 1.2 m diameter - 3mm stainless 50 km of weld 10-9 torr vacuum and no leaks! Seismic isolation Stack of masses and springs Coils and magnets to control the mirror Fused silica mirror 25 cm diameter 10 kg mass
18 Hanford Detektor
19
20 LIGO, Hanford
21
22 LIGO, Hanford
23 LIGO, Livingston
24
25
26
27 LIGO Livingston
28
29 The Need for Advanced LIGO Initial LIGO Goal: factor of ten improvement in sensitivity at all frequencies E-LIGO x10 increase in sensitivity = x1000 volume of sky searched Inspiral event rate from one every few years to one every few days!
30 New Optic Suspensions 40 kg fused silica optics Quadruple suspension with reaction mass Last stage suspended by fused silica ribbons for higher Q
31 Derzeit wird Advanced-LIGO aufgebaut (bis 2014) 10 größere Sensitivität Aufhängung der Spiegel (40 kg) mittels Fasern
32 GEO600
33 GEO600
34 GEO600
35 GEO600 Aufhängung
36 GEO600
37 AIGO Astralian Internationel Gravitational Observatory
38
39 AIGO
40 TAMA300
41
42 TAMA300
43 Laser Interferometer Space Antenna (LISA)
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