Finding Black Holes with Lasers
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1 Finding Black Holes with Lasers Andreas Freise Royal Institute of Great Brtitain [Image shows guide laser at Allgäu Public Observatory in Ottobeuren, Germany. Credit: Martin Kornmesser] LIGO-G
2 Astronomy A. Freise 2
3 Big Science A. Freise 3 ASKAP, part of SKA [
4 LIGO Laser Interferometer Gravitational wave Observatory
5 LIGO Laser Interferometer Gravitational wave Observatory Gravitational Waves! an exemplary (personal) story...
6 Gravitational what?
7
8 96% of the Universe
9 Gravitational Waves A fundamental prediction of general relativity Ripples of space-time that propagate at the speed of light Produced by large, compact and relativistic concentration of mass or energy Stretch and squeeze space A. Freise 8
10 Einstein s theory of relativity G µ = 8 G c 4 T µ A. Freise 9
11 Generation of GWs The Claw, Dreamworld Australia Binary black hole merger L ~ W L ~ 10, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000, 000 W A. Freise 10
12 Sources of Gravitational Waves binary systems Any mass distribution that is accelerated in a non-spherically symmetric way (waving hands, running trains, planets in orbit, ) Large masses necessary to get any measurable signal supernovae pulsars accreting stars A. Freise 11
13 Gravitational waves from merging black holes A. Freise Baker, NASA GSFC 12
14 Bobbing like a Cork... [Credit: A. Freise 13
15 And the big question: [Credit: A. Freise 15
16 Gravitational Wave Detection! A. Freise 16
17 Observing Gravitational Waves: Laser Interferometers Δ L ~ L x h h =10-22 is tiny!! A. Freise 17
18 Interferometry in 1887 Michelson interferometer (ca. 1887) Sensitivity: 0.01 of a fringe A. Freise 18
19 Interferometry in 1972 MIT Sensitivity: of a fringe Rai Weiss, MIT A. Freise 19
20 GW interferometry today LIGO-Hanford (H1: 4 km, H2: 2 km) Sensitivity: of a fringe or size of a nucleus A. Freise 20
21 World-wide Network LIGO Hanford 4km GEO m Virgo 3km LIGO India (planned) KAGRA 3km (under construction) LIGO Livingston 4km A. Freise 21
22 The Emergence of a New Science A. Freise 22
23 The First Generation GEO, TAMA, Virgo, LIGO Proposed in the 1980ies Development of new technologies Detectors build in the 1990ies Development of even newer technologies Operation and data taking A. Freise 23
24 The First Generation GEO, TAMA, Virgo, LIGO Proposed in the 1980ies Development of new technologies Detectors build in the 1990ies Development of even newer technologies Operation and data taking A. Freise 23
25 GEO 600 (British/German) [Credit: Albert-Einstein Institute / GEO 600] A. Freise 24
26 A GEO600 Mirror Suspension A. Freise 25
27 GEO 600 control room (2001) A. Freise 26
28 Virgo airial view [Credit: A. Freise 27
29 Virgo Main Optics High quality fused-silica mirrors 35 cm diameter, 10 cm thick Substrate losses 1 ppm Coating losses <5 ppm Surface deformation λ/100 (rms on 150mm) [Credit: A. Freise 28
30 Virgo Control Room (2003) A. Freise 29
31 2012
32 Result? No gravitational wave yet! We learned a lot! Global gravitational wave community A. Freise 31
33 Advanced LIGO A. Freise 32
34
35 Upgrade of existing LIGO Start of operation >2015 A. [Credit: FreiseLIGO Laboratory] 34
36 Advanced Interferometry A. Freise
37 Michelson used his eye to measure the light, this is how one photo detection port looks today: Main Interferometer Beam External bench [Credit:
38 A. [Credit: FreiseLIGO Laboratory] 37
39 David Willetts, Minister of State for Universities and Science A. Freise 38 IOP [Credit: Lecture John James]
40 Advanced LIGO is expected to achieve first detection! What shall we do then?
41 Preparing for Advanced LIGO Commissioning and Simulation Workshop, LIGO Livingston A. Freise
42 The `Arm Cavity [Images: Virgo, and LIGO Laboratory] A. Freise 41
43 The `Arm Cavity [Images: Virgo, and LIGO Laboratory] A. Freise 41
44 The `Arm Cavity [Images: Virgo, and LIGO Laboratory] A. Freise 41
45 The `Arm Cavity [Images: Virgo, and LIGO Laboratory] A. Freise 41
46 The Mirror Surface [Images: Virgo, and LIGO Laboratory] Surface measurement
47 Beam shape distortions Acceptance of mirrors from manufacturer: Computer model is used to estimate the optical distortions due to the measured mirror distortions. Beam shape inside arm cavity A. Freise
48 FINESSE: Open Source Simulation Started in 1997 and developed as my PhD side project, used extensively worldwide Versions available for Windows, Linux and Mac OSX, open source, download at 44
49 Reflection from the Advanced LIGO pre-modecleaner cavity, image by Kate Dooley
50 The Einstein Telescope A. Freise 46
51
52 Large Infrastructure [M. Doets, D. Rabeling] A. Freise 48
53 Large Infrastructure [M. Doets, D. Rabeling] A. Freise 48
54 Large Infrastructure [M. Doets, D. Rabeling] Hello! Can you see me? A. Freise 48
55 A. Freise 49 IOP Lecture [M Doets, D. Rabeling]
56 A. Freise 50 IOP Lecture [M Doets, D. Rabeling]
57 A. Freise 51
58 Science is a slow process You can have a big impact A. Freise 52
59 ...end A. Freise 53
60 Acknowledgements Some of the images and media shown were produced by these gravitational wave projects: LIGO Laboratory and the LIGO Scientific Collaboration, GEO 600, Virgo, Einstein Telescope, LISA, KAGRA, Further support and material has been provided by the following institutions: Gravitational Wave Group University of Birmingham, Albert Einstein Institute, NIKHEF, Numerical Relativity group, FSU Jena, NASA, GSFC, Caltech-Cornell, A. Freise 54
61 Image Credits Individual images were produced by: Martin Kornmesser (ESO) Ant Schinckel (CSIRO) T. Carnahan (NASA GSFC) Lainey Bird Sky and Telescope Magazine John James Kate Dooley (LIGO/GEO) Martin Doets, David Rabeling (Nikhef) A. Freise 55
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