Barry C Barish LIGO Laboratory 1Sept2017 17Aug17 PAX Workshop Amsterdam 2 Context of G3 Where will we be Particle Physics 17Aug17 PAX Workshop Amsterdam 3 Gravitational Waves ID: 811295
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Slide1
GW Policy: The Future: G3 Detectors
Barry C BarishLIGO Laboratory 1-Sept-2017
Slide217-Aug-17PAX Workshop - Amsterdam
2
Context of G3: Where will we be?
Slide3Particle Physics17-Aug-17
PAX Workshop - Amsterdam3
Slide4Gravitational Waves17-Aug-17
PAX Workshop - Amsterdam4
Slide5Primary Tools17-Aug-17
PAX Workshop - Amsterdam5
Particle PhysicsAccelerators
Gravitational Waves
Interforometers
Slide6General Structures
IUPAP / C11 – ICFACommunity ~ 10 KTheory / ExperimentLarge FacilitiesAccelerator R&D
‘Closed’ Scientific CollaborationsMultiple Instruments for ‘Confirmation’IUPAP / GWICCommunity ~ 1.5 KTheory / Experiment
Large Facilities
Interferometer R&D
‘Open’ Scientific Collaborations
Multiple Instruments for ‘Scientific Capability’
17-Aug-17
PAX Workshop - Amsterdam
6
Slide77
Einstein’s Theory of Gravitation
Gravitational Waves
Using
Minkowski
metric, the information about space-time curvature is contained in the metric as an added term,
h
mn
. In the weak field limit, the equation can be described with linear equations. If the choice of gauge is the
transverse traceless gauge
the formulation becomes a familiar wave equation
The strain
h
mn
takes the form of a plane wave propagating at the speed of light (c).
Since gravity is spin 2, the waves have two components, but rotated by 45
0
instead of 90
0
from each other
.
August 2017
Pontecorvo Summer School
Slide8Pontecorvo Summer School
8
LIGO detectors are nearly
omni
-directional
Individually they provide almost no directional information
Array working together can determine source location using timing and amplitudes
Source Localization
Using
Time-of-flight
August 2017
Slide9Localization LIGO O1 Events
12-July-20179
Christodoulou - ETH ZurichSimulation for 3rd detector at Virgo location with LIGO O1 sensitivity
Slide1010
GW detector network:
2015-2025
GEO600 (HF)
2011
Advanced LIGO
Hanford
2015
Advanced LIGO
Livingston
2015
Advanced
Virgo
2016
LIGO-India
2022
KAGRA
2017
August 2017
Pontecorvo Summer School
10
Slide11Improving Localization
2016-17
2017-182019+
2024
August 2017
Pontecorvo Summer School
11
LIGO-P1200087-v32
(Public)
Slide12G3: Some Big IssuesScience Motivations and Goals
GWIC Committee (must be done in the context of projected G2)Science Goals Technical Performance
Frequency vs Sensitivity Goals?Network Performance Goals (e.g. Pointing Accuracy)?Strategic IssuesHow many G3 Detectors are required?
Features/Priorities: Sensitivity vs Frequency; Polarization; Network
G3 Detectors: Identical or Different?
How Internationally Organized/Funded/Implemented?
Present GW Model: “Collaboration of Collaborations?”
Globally Organized, like ILC, SKA?
Global w/ Strong Host, like CERN LHC, DUNE?
‘Limited’ Partnerships, like ALMA, LSST, TMT?
17-Aug-17
PAX Workshop - Amsterdam
12
Slide13KAGRA
Kamioka Mine
Underground
Cryogenic Mirror
Technologies crucial for next-generation detectors;
KAGRA can be regarded as a 2.5-generation detector.
Slide14GWIC – 3G Science Case17-Aug-17
PAX Workshop - Amsterdam14
Slide15The GWIC Committee17-Aug-17
PAX Workshop - Amsterdam15
Slide16Top Level Science Questions17-Aug-17
PAX Workshop - Amsterdam16
Slide17Mature 3G Concept
LASER
Advanced
LIGO
4 km
Einstein
Telescope
10 km
The Einstein Telescope: x10 aLIGO
Deep Underground;
10 km arms
Triangle (polarization)
Cryogenic
Low frequency configuration
high frequency configuration
17
17-Aug-17
PAX Workshop - Amsterdam
Einstein Telescope
Slide18Preliminary Concept
LASER
Advanced
LIGO
4 km
18
17-Aug-17
PAX Workshop - Amsterdam
Cosmic Explorer
The
Cosmic Explorer:
x10 aLIGO
Earth‘s Surface;
40
km arms
Advanced LIGO Technology +
Squeezed Light
Cosmic Explorer
40
km
arXiv:1607.08697v3 [astro-ph.IM] 11 Sep 2016
Slide193G R&D Critical r & D
Initial / Adv LIGO/Virgo Technical Developments3G -- New Technical Developments:
PAX Amsterdam19
Longer arms
Squeezed quantum states
Lower thermal noise coatings
Low noise cryogenics
Newtonian noise cancellation
Adaptive controls
Fabry
-Perot arm cavities
Laser stabilization
Diode-pumped
Nd:YAG
lasers
Supermirrors (polishing and coatings)
Multi-stage active seismic isolation
Fused silica suspensions
Digital control systems
Slide20Next Steps (~5 years)
Science Case (GWIC study + …..)Top-level Technical Requirements and priorities Detector Concepts (ET, CE or ??) Based on technical requirements set by Science Case
Global Concept for “3G”How many detectors? How different??Define required technology R&D neededEstimate costs (minimal system, options, etc)Define global organization or coordination
Politics:
Other physicists / scientists; public;
funding agencies
Submit Funding Proposal(s)
PAX Amsterdam
20
17-Aug-2017