Challenges in designing interferometric. Andreas Freise
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1 Laser Ranging Challenges in designing interferometric in a gravitational new Dimension wave detectors Andreas Freise with contributions from Daniel Brown, Daniel Töyrä and the LIGO-Virgo Collaboration LIGO document number: LIGO-G
2 Download on the app store (ios, Android) or via the webpage: Tweet a photo with hashtag #PyDataLondon
3 In the News: [Photo by Kate Gushwa, Matt Heintze, Calum Torrie and Liz Natividad] A. Freise 3
4 A. Freise 4
5 Astronomy A. Freise 5
6 Hubble Space Telescope A. [Image: Freise NASA] 6
7 [NASA, ESA, Z. Levay (STScI), T. Rector, I. Dell'Antonio/NOAO/AURA/NSF, G. Illingworth, D. Magee, and P. Oesch (University of California, Santa Cruz), R. Bouwens (Leiden University) and the HUDF09 Team]
8 [NASA, ESA, Z. Levay (STScI), T. Rector, I. Dell'Antonio/NOAO/AURA/NSF, G. Illingworth, D. Magee, and P. Oesch (University of California, Santa Cruz), R. Bouwens (Leiden University) and the HUDF09 Team]
9 [Credit: NASA and the Night Sky Network] Life Cycle of Stars
10 The Sun Size = 109 Earth Mass = Earth
11 The Sun Size = 109 Earth Mass = Earth Earth and Moon
12 Neutron Stars and Black Holes Birmingham Neutron Star Black Hole
13 What are Black Holes?
14
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16 Einstein s Theory of Relativity Einstein, Die Grundlage der allgemeinen Relativitätstheorie A. Freise 13
17 Gravitational Waves Two black holes circling around each other (a binary system).. create a very strong and quickly varying gravitational field and ripples in spacetime that run away at the speed of light. A. Freise
18 Astronomy A. Freise 15
19 Gravitational Wave Astronomy A. Freise 15
20 Observing Gravitational Waves: Gravitational waves change the distance between objects. [ A. Freise 16
21 Observing Gravitational Waves: Gravitational waves change the distance between objects. [ A. Freise 16
22 Observing Gravitational Waves: Gravitational waves change the distance between objects. [ A. Freise 16
23 Laser Rangefinder Wikipedia on Rangefinders: The precision of the instrument is determined by the rise or fall time of the laser pulse and the speed of the receiver. One that uses very sharp laser pulses and has a very fast detector can range an object to within a few millimeters. A. Freise 17
24 Length Measurement with Light Use a reference beam instead of a clock An interferometer compares two light beams Output becomes dark or bright when the light beams shift A. Freise 18
25 Length Measurement with Light Use a reference beam instead of a clock An interferometer compares two light beams Output becomes dark or bright when the light beams shift A. Freise 18
26 Interferometry in 1887 Michelson interferometer (ca. 1887) Sensitivity: 0.01 of a fringe 1 fringe A. Freise 19
27 Length Scales µ A. Freise 20
28 Length Scales µ A. Freise 21
29 Length Scales µ Michelson 1887 A. Freise 21
30 Length Scales µ Michelson 1887 Gravitational Waves A. Freise 21
31 Two LIGO Instruments H1 10 ms light travel time Sensitivity: of a fringe L1 or m
32 LIGO Laser Interferometer Gravitational-Wave Observatory Two large Michelson interferometers! How does one instrument look like? A. Freise 23
33 LIGO Hanford Site A. Freise 24
34 [Images: Google Earth and LIGO]
35 [Images: Google Earth and LIGO]
36 [Images: Google Earth and LIGO]
37 [Images: Google Earth and LIGO]
38 [Images: Google Earth and LIGO]
39 [Images: Google Earth and LIGO]
40 [Images: Google Earth and LIGO]
41 [Images: Google Earth and LIGO]
42 [Images: Google Earth and LIGO]
43 [Images: Google Earth and LIGO]
44 First Detection of Gravitational Waves A. Freise 30
45 Data recorded on the 14th of September 2015, at 09:50:45 UTC A. Freise 31
46
47
48 Fact sheet About 1 billion years ago (1 billion light years away), two black holes merged Before: two black holes of 36 and 29 solar masses After: one black hole, 62 solar masses Inspiral and merge is a very violent event, rotation speed up to 200 Hz Last year the LIGO mirrors wiggled by meters for 0.1 seconds A. Freise 33
49 Three Key Results First direct detection of a gravitational wave, confirmation of Einstein s prediction. Discovery of the first binary black hole. Strongest evidence so far that Nature s black holes are those described by general relativity. The start of a new era in astronomy! A. Freise 34
50 Part 2 How to build such an amazingly sensitive laser interferometer? A. Freise 35
51 LIGO Scientific Collaboration
52 Advanced Interferometry A. Freise
53 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities A. Freise 38
54 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: km high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities A. Freise 38
55 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: km high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities A. Freise 38
56 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: km high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities A. Freise 38
57 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: km high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities Stop everything from shaking! A. Freise 38
58 What Makes it Better? GW effect scales with arm length: large detectors Optical signal scales with light power: km high-power laser, optical cavities Laser beam fluctuations make noise: filter cavities Stop everything from shaking! A. Freise 38
59 Complexity Increases Michelson used his eye to measure the light, this is how one photo detection port looks now: Main Interferometer Beam [Image: Virgo Collaboration] A. Freise 39
60 10 to 30 Years from Idea to Application Numerical simulations Idea Analytic computations Detector system construction Detector commissioning Table-top tests Prototype interferometers A. Freise 40
61 Linear Interaction of Light with Optics A. Freise 41
62 Optical Systems as a Sparse Matrix A. Freise 42
63 Play and Evolve Spare matrix solvers are available, so what is the problem? Commercial software is not aimed at optical phase changes of and interference effects at that level We are building a completely new class of device, there is no manual, everything is new, we learn as we go along It is easy to make plots of interferometer signals, but it is hard to ask the right questions A LIGO detector is a strongly coupled assembly of many optical parts, the interplay between different parts caused surprises! A. Freise 43
64 Adapt Complexity Correctly Model everything in detail to replicate your experiment in the computer? No, model output as difficult to understand as real experiment. Use fundamental concepts only? No, your model will not reproduce the behaviour that you want to investigate. Use the right level of abstraction and allow to add or remove details? Yes, your model mimics the real instrument, but has less complexity! A. Freise 44
65 Invented here Software developed as side project by scientist working on non-code tasks Developer is its own user, often the only one Code quality is low, best practises are not known or not followed Difficult to make impact in teams or projects `real physicists don t use simulations A. Freise 45
66 FINESSE Started 1997 as a PhD side project o_.- =. (\'".\.>' (_- -. Stand- alone binary, written in C > lines of code Open sourced in 2012 _=/d,^\ Under active development ~~ \)- ' ' Used extensively worldwide / '- - ' A. Freise 46
67 User interface Measurement of radiation-pressure-induced optomechanical dynamics in a suspended Fabry-Perot cavity Corbitt, et. al A. Freise 47
68 User interface Measurement of radiation-pressure-induced optomechanical dynamics in a suspended Fabry-Perot cavity Corbitt, et. al A. Freise 47
69 User interface Measurement of radiation-pressure-induced optomechanical dynamics in a suspended Fabry-Perot cavity Corbitt, et. al A. Freise 47
70 User interface Measurement of radiation-pressure-induced optomechanical dynamics in a suspended Fabry-Perot cavity Corbitt, et. al A. Freise 47
71 FINESSE 1.0 download locations A. Freise 48
72 From Matlab to Python We needed a scripting environment to support the stand-alone simulation software to: automate simulation tasks pre- and post-processing of data present results of complex tasks 2006 developed a set of tools to run FINESSE from Matlab 2013 started to develop PyKat, a Python-based replacement A. Freise 49
73 Why Python? Originally used Matlab because is has been chosen as the standard tool of the project, but Matlab licenses are expensive, artificially limits the reach of our software Many features of the framework require text parsing, which is difficult in Matlab Python is cool, students want to use it Python (now) provides the right mixture of stability and playground A. Freise 50
74 PyKat Python- based tools for optical..- _ '( \`. \....- """"- _." ) _ / ' `.- '. ' `: 7/* _/._\ \ ( ( '::;;+;;: `- "' =" /,`"" `) / L. \`:::a:f c_/ n_'..` `.., `^-... : +. simulations Primary use: IPython notebooks to run FINESSE simulations Python 2/3 compatible main packages used: NumPy, Matplotlib, SciPy, SymPy A. Freise 51
75 Finesse at work A. [Logbook Freise page 2292, , Holger Wittel] 52
76 Simulations during operations Availability of well tested, `realistic models Modelling interferometer response to signals and to noise for calibration and noise budget Identifying unexpected features, to make use of them as diagnostic tools Capability to investigate proposed changes before hardware changes A. Freise 53
77 A long time ago, in the GEO 600 control room A. Freise 54
78 Distorted Control Signals A. Freise 55
79 Distorted Control Signals end mirrors with wrong curvature A. Freise 55
80 Distorted Control Signals end mirrors with wrong curvature A. Freise 55
81 Distorted Control Signals end mirrors with wrong curvature BS `tilt motion excited A. Freise 55
82 Distorted Control Signals end mirrors with wrong curvature BS `tilt motion excited A. Freise 55
83 LIGO Mirrors A. Freise 56
84 LIGO Mirror Surface Quality LIGO mirrors require extremely flat surfaces aligo map ETM08: central 30cm rms = 0.52nm Surface roughness or distortions cause optical loss, details depend on the type and shape of the distortions Surface measurement are available from manufacturer aligo map ETM08: central 16cm rms = 0.17nm Numerical modelling is used to predict optical loss to determine if mirrors can be accepted A. Freise 57
85 Teaching and Training A. Freise 58
86 Teaching a New Generation In 2015/2016 we ran two successful summer school for post-graduate students Teaching material entirely based on IPython notebooks Installed all software on user-owned laptops, using Anaconda teaching laser interferometry, quantum optics, modelling Now moving this material online A. Freise 59
87 A. Freise 60
88 Does Python work for us? Pros: Easy to learn, fun to use Free, cross platform Powerful and flexible Facilitates transparency, sharing, and teaching Cons: Installation not trivial, often the show stopper for new users Variants of documentation and packages are confusing Lack of specific Matlab package Simulink for control systems A. Freise 61
89 More Python in LIGO Automation and control of the LIGO detectors: J.G. Rollins `Distributed State Machine Supervision for Long-baseline Gravitational-wave Detectors, Data analysis, see for example the IPython notebook in the open data release of the first detection: GW150914_tutorial.html [Image from the film LIGO, A Passion for Understanding by Kai Staats] A. Freise 62
90 Find out more!
91 Find out more!
92 ...end A. Freise 64
93
94 Ground-based detectors today LIGO Hanford 4km GEO m Virgo 3km LIGO India (planned) KAGRA 3km (under construction) LIGO Livingston 4km A. Freise 66
95 The full GW spectrum (Credits: Ira Thorpe)
96 Advanced LIGO Parameters A. Freise 68
97 [Sketch by Nutsinee Kijbunchoo] A. Freise 69
98 Einstein publishes new theory of gravity, predicting gravitational waves 1915/ 1916 Joseph Weber constructs resonant bar GW detectors Nobel Prize for Hulse and Taylor, indirect proof for existence of GWs Rainer Weiss and Robert Forward start working on interferometric detectors 1960s 1970s 1993 LIGO is founded scientific data taking periods with LIGO, Virgo, GEO and TAMA, without a detection Upgrade of LIGO detectors, for a 10-fold increase in sensitivity Bringing LIGO to its new design sensitivity A. Freise 70 Today
99 Einstein publishes new theory of gravity, predicting gravitational waves 1915/ 1916 Joseph Weber constructs resonant bar GW detectors Nobel Prize for Hulse and Taylor, indirect proof for existence of GWs Rainer Weiss and Robert Forward start working on interferometric detectors 1960s 1970s 1993 LIGO is founded scientific data taking periods with LIGO, Virgo, GEO and TAMA, without a detection A. Freise Today Upgrade of LIGO detectors, for a 10-fold increase in sensitivity Bringing LIGO to its new design sensitivity Detections!
100 Life and Death of Simulations [Talk by Jerome Degallaix, LIGO commissioning and simulation workshop, Feb. 2013] A. Freise 71
101 A GEO600 Mirror Suspension 72 A. Freise
102 Beam Shape Distortions Acceptance of mirrors from manufacturer: Computer models are used to estimate the optical distortions due to the measured mirror distortions. 73 Beam shape inside arm cavity A. Freise
103 Beam Shape Distortions Acceptance of mirrors from manufacturer: Computer models are used to estimate the optical distortions due to the measured mirror distortions. 73 Beam shape inside arm cavity A. Freise
104 LIGO commissioning, task sharing and recording A. Freise 74
105 Why Interferometer Simulations? Investigation of new interferometry techniques, or new optical technologies Optical design of the gravitational wave detectors, computation of requirements for optical components Commissioning of the detectors A. Freise 75
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