LIGO-IndiaDetecting Einstein’s Elusive Waves

Opening a New Window to the Universe

An Indo-US joint mega-project concept proposal

IndIGO Consortium(Indian Initiative in Gravitational-wave Observations)

Version: 3 Jun 11, 2011www.gw-indigo.org

In 1916, Albert Einstein published his famous Theory of General Relativity, the theory of gravitation.4-dimensional space-time (the normal three dimensions of space, plus a fourth dimension of time).

His theory describes how space-time is affected by mass and also how mass affects spacetime. Matter tells spacetime how to curve, and spacetime tells matter how to move.

Space Time as a fabric

Space Time as a fabric

Einstein’s General theory of relativity is the most beautiful & successful theory of modern physics. It has matched all tests of Gravitation in the solar system (weak fields) remarkably well.

What happens when matter is in motion?

Einstein’s theory predicts

Matter in motion fluctuation in the curvature of space-time which propagates as a waveSpace-time ripples or gravitational waves

Binary Neutron stars

Pulsar companion

GW from Binary Neutron stars

1. leads to loss of orbital energy

2. period speeds up 14 sec from 1975-94

3. measured to ~50 msec accuracy

4. deviation grows quadratically with time

Binary pulsar emits gravitational waves Hulse and TaylorResults for PSR1913+16

Indirect evidence for Gravity waves

Nobel prizein 1993 !!!

Effect of GW on test masses

Effect of GW on a ring of test masses

Interferometer mirrors as test masses

Detecting GW with Laser Interferometer

Difference in distance of Path A & B Interference of laser light at the detector (Photodiode)

Path A

Path B

A B

The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer.

Equal arms: Dark fringe

Unequal arm: Signal in PD

Path difference phase difference

Challenge of Direct Detection

2 L hL

20 2310 10h

Gravitational wave is measured in terms of strain, h(change in length/original length)

Expected amplitude of GW signals

Measure changes of

one part in thousand-billion-billion!

Gravitational waves are very weak!

A Century of Waiting• Almost 100 years since Einstein predicted GW but no direct

experimental confirmation a la Hertz• Two Fundamental Difference between GR and EM- Weakness of Gravitation relative to EM (10^-39)-Spin two nature of Gravitation vs Spin one of EM that forbids

dipole radiation in GR-Low efficiency for conversion of mechanical energy to GW.

Feeble effects of GW on a Detector• GW Hertz expt ruled out. Only astrophysical systems involving

huge masses and accelerating very strongly are potential sources of GW signals.

LIGO and Virgo TODAYField reached a Milestone with decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide

Unprecedented sensitivity allows one to place Upper Limits on GW from a variety of Ap sources. Improve on Spindown of Crab, Vela pulsars, Big Bang nucleosynthesis bound on Stochastic GW..

Schematic Optical Design of Advanced LIGO detectors

Expected Annual Coalescence RatesIn a 95% condence interval, rates uncertain by 3 orders of magnitudeNS-NS (0.4 - 400); NS-BH (0.2 - 300) ; BH-BH (2 - 4000) yr^-1Based on Extrapolations from observed Binary Pulsars,Stellar birth rateestimates, Population Synthesis models. Rates quoted below are mean of the distribution.

Detector Generation

NS-NS NS-BH BH-BH

Initial LIGO(2002 -2006) 0.02 0.0006 0.0009

Enhanced LIGO(2X Sensitivity)(2009-2010)

0.1 0.04 0.07

Advanced LIGO(10X sensitivity)(2014 - …)

40 10. 20.0

Era of Advanced LIGO detectors: 2015

10x sensitivityÞ10x reach

Þ 1000 volume>> 1000 event

rate(will reach beyond

nearest superclusters )

GW Astronomy with Intl. Network of GW Observatories

LIGO-LLO: 4km

LIGO-LHO: 2km, 4kmGEO: 0.6km VIRGO: 3km

LCGT 4kmTAMA/CLIO

LIGO-Australia?

1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info.

LIGO-India ?

Courtesy: B. Schutz: GWIC Roadmap Document

GWIC: Gravitational Wave International Committee

Indo-Aus.Meeting, Delhi, Feb 2011

Courtesy: B. Schutz, GWIC Roadmap Document 2010

Gravitational wave Astronomy :Synergy with other major Astronomy projects:

• SKA: Radio : Pulsars timing, • X-ray satellite (AstroSAT)• Gamma ray observatory• Thirty meter telescope: gamma ray follow-up,…• •

INDIGO: the goals• Major experimental science science initiative in GW astronomy

LIGO-India (Letter from LIGO Labs)– Advanced LIGO hardware for 1 detector to be shipped to India.– India provides suitable site and infrastructure to house the GW observatory– Site, two 4km armlength high vacuum tubes in L config.– Indian cost ~Rs 1000Cr Earlier plan: Partnership in LIGO-Australia (a diminishing possibility)

– Advanced LIGO hardware for 1 detector to be shipped to Australia at the Gingin site, near Perth. NSF approval– Australia and International partners find funds (equiv to half the detector cost ~$140M and 10 year running cost ~$60M) within a year.– Indian partnership at 15% of Australian cost with full data rights.

• Consolidated IndIGO membership of LIGO Scientific Collaboration + propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint Centre at

IUCAA with Caltech (funded)

• Provide a common umbrella to initiate and expand GW related experimental activity and training new manpower – 3m prototype detector in TIFR (funded). Unnikrishnan– Laser expt. RRCAT, IIT M, IIT K | High Vaccum & controls at RRCAT, IPR, BARC, ISRO, ….– UG summer internship at Natn. & Intl GW labs & observatories.– Postgrad IndIGO schools, specialized courses,…

Multi-Institutional,Multi-disciplinary Consortium

1. CMI, Chennai2. Delhi University3. IISER Kolkata4. IISER Trivandrum5. IIT Madras6. IIT Kanpur7. IUCAA8. RRCAT9. TIFR

• RRI• IPR, Bhatt• Jamia Milia Islamia• Tezpur Univ

The IndIGO Consortium

Data Analysis & Theory

1. Sanjeev Dhurandhar IUCAA2. Bala Iyer RRI3. Tarun Souradeep IUCAA4. Anand Sengupta Delhi University 5. Archana Pai IISER, Thiruvananthapuram6. Sanjit Mitra JPL , IUCAA7. K G Arun Chennai Math. Inst., Chennai8. Rajesh Nayak IISER, Kolkata9. A. Gopakumar TIFR, Mumbai 10. T R Seshadri Delhi University 11. Patrick Dasgupta Delhi University12. Sanjay Jhingan Jamila Milia Islamia, Delhi13. L. Sriramkumar, Phys., IIT M14. Bhim P. Sarma Tezpur Univ . 15. P Ajith Caltech , USA16. Sukanta Bose, Wash. U., USA17. B. S. Sathyaprakash Cardiff University, UK18. Soumya Mohanty UTB, Brownsville , USA19. Badri Krishnan Max Planck AEI, Germany

Instrumentation & Experiment

1. C. S. Unnikrishnan TIFR, Mumbai2. G Rajalakshmi TIFR, Mumbai3. P.K. Gupta RRCAT, Indore 4. Sendhil Raja RRCAT, Indore5. S.K. Shukla RRCAT, Indore6. Raja Rao ex RRCAT, Consultant 7. Anil Prabhakar, EE, IIT M8. Pradeep Kumar, EE, IIT K9. Ajai Kumar IPR, Bhatt10. S.K. Bhatt IPR, Bhatt 11. Ranjan Gupta IUCAA, Pune12. Rijuparna Chakraborty, Cote d’Azur, Grasse13. Rana Adhikari Caltech, USA 14. Suresh Doravari Caltech, USA 15. Biplab Bhawal (ex LIGO)

IndIGO Council1. Bala Iyer ( Chair) RRI,

Bangalore 2. Sanjeev Dhurandhar (Science) IUCAA, Pune 3. C. S. Unnikrishnan (Experiment) TIFR, Mumbai4. Tarun Souradeep (Spokesperson) IUCAA, Pune

Committees: National Steering Committee:Kailash Rustagi (IIT, Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]D.D. Bhawalkar (Quantalase, Indore)[Advisor]P.K. Kaw (IPR)Ajit Kembhavi (IUCAA) P.D. Gupta (RRCAT)J.V. Narlikar (IUCAA)G. Srinivasan

International Advisory Committee

Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO, Caltech, USA)David Blair (AIGO, UWA, Australia)Adalberto Giazotto (Virgo, Italy)P.D. Gupta (Director, RRCAT, India)James Hough (GEO ; Glasgow, UK)[GWIC Chair]Kazuaki Kuroda (LCGT, Japan)Harald Lueck (GEO, Germany)Nary Man (Virgo, France)Jay Marx (LIGO, Director, USA)David McClelland (AIGO, ANU, Australia)Jesper Munch (Chair, ACIGA, Australia)B.S. Sathyaprakash (GEO, Cardiff Univ, UK)Bernard F. Schutz (GEO, Director AEI, Germany)Jean-Yves Vinet (Virgo, France)Stan Whitcomb (LIGO, Caltech, USA)

IndIGO Advisory Structure

Program Management committee

C S Unnikrishnan (TIFR, Mumbai), Chair.Bala R Iyer (RRI, Bangalore), CoordinatorSanjeev Dhurandhar (IUCAA, Pune) Co-cordinatorTarun Souradeep (IUCAA, Pune)Bhal Chandra Joshi (NCRA, Pune)P Sreekumar (ISAC, Bangalore)P K Gupta (RRCAT, Indore)S K Shukla (RRCAT, Indore)Sendhil Raja (RRCAT, Indore)

INSERT BOX

LIGO-Australia: Idea and Opportunity

• The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site, W. Australia to maximize science benefits like baseline, pointing, duty cycle, technology development and international collaboration.

• The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity.

- Indian contribution in hardware (end station vacuum system, and controls), Data centre, manpower for installation and commissioning.

Indo-US centre for Gravitational Physics and Astronomy

• Centre of Indo-US Science and Technology Forum (IUSSTF)

• Exchange program to fund mutual visits and facilitate interaction.

• Nodal centres: IUCAA , India & Caltech, US.

• Institutions:

Indian: IUCAA, TIFR, IISER, DU, CMI - PI: Tarun Souradeep US: Caltech, WSU - PI: Rana Adhikari

APPROVED for funding (Dec 2010)

The IndIGO data analysis centre

• Tier -2 centre with data archival and computational facilities

• Inter-institutional proposal for facility

• Propose for a high-throughput Computation and GW Data Archival Centre.

• Will provide fundamental infrastructure for consolidating GW data analysis expertise in India.

Tier 0 •LIGO Sites at Hanford, Livingston •Data acquisition systems

Tier 1 •LIGO Labs at Caltech

Tier 2 •LIGO Lab at MIT, LSC institutions like UWM, Syracuse etc

•IndIGO Data Analysis Centre

Courtesy: Anand Sengupta

Objectives of the data centre

Tier 2Data Centre

at IUCAA

Archival

Communitydevelopment

Indian Researchers and Students

TIER3 centres at Univ & IISERS

Other science groups

Web ServicesCollaboration

tools

Analysis

LSCLIGO Data Grid

LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre.

Courtesy: Anand Sengupta

Primary Science: Online Coherent search for GW signal from binary mergers using data from global detector network

Role of IndIGO data centre Large Tier-2 data/compute centre for archival of g-wave data and analysis Bring together data-analysts within the Indian gravity wave community. Puts IndIGO on the global map for international collaboration with LIGO

Science Collab. wide facility. Part of LSC participation from IndIGO

• 100 Tflops = 8500 cores x 3 GHz/coreNeed 8500 cores to carry out a half decent coherent search for gravitational waves

from compact binaries.(1 Tflop = 250 GHz = 85 cores x 3 GHz / core)

• Storage: 4x100TB per year per interferometer.• Network: gigabit backbone, National

Knowledge Network. Courtesy: Anand Sengupta, IndIGO

IndIGO Data Centre@IUCAA Indian Initiative in Gravitational-wave Observations

23 July 2011Dear Bala:

I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO. This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO. Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membership……

In its road-map with a thirty year horizon, the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics, IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations. We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium, for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site. In what follows this project is referred to as LIGO-India. The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories.

LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave observatories now being installed the US (LIGO) and in Europe (Virgo and GEO) and would be of great value not only to the gravitational wave community, but to broader physics and astronomy research by launching an era of gravitational wave astronomy, including, the fundamental first direct detection of gravitational waves. As the southernmost member observatory of the global array of gravitational wave detectors, India would be unique among nations leading the scientific exploration of this new window on the universe. The present proposal promises to achieve this at a fraction of the total cost of independently establishing a fully-equipped and advanced observatory. It also offers technology that was developed over two decades of highly challenging global R&D effort that preceded the success of Initial LIGO gravitational wave detectors and the design of their advanced version.

LIGO-India

LIGO-India: Why is it a good idea?for India

• Has a 20 year legacy and wide recognition in the Intl. GW community with seminal contributions to Source modeling (RRI)& Data Analysis (IUCAA). High precision measurements (TIFR), Participation in LHC (RRCAT)

• (Would not make it to the GWIC report, otherwise!)– AIGO/LIGO/EGO strong interest in fostering Indian community– GWIC invitation to IndIGO join as member (July 2011)

• Provides an exciting challenge at an International forefront of experimental science. Can tap and siphon back the extremely good UG students trained in India. (Sole cause of `brain drain’).

– 1st yr summer intern 2010 MIT for PhD– Indian experimental scientist Postdoc at LIGO training for Adv. LIGO subsystem

• Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India.

– Sendhil Raja, RRCAT, Anil Prabhakar, EE, IIT Madras, Pradeep Kumar, EE, IITK Photonics– Vacuum expertise with RRCAT (S.K. Shukla, A.S. Raja Rao) , IPR (S.K. Bhatt, Ajai Kumar)

• Jump start direct participation in GW observations/astronomy – going beyond analysis methodology & theoretical prediction --- to full fledged participation in

experiment, data acquisition, analysis and astronomy results.

• For once, may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed. Once in a generation opportunity to host an Unique International Experiment here.

LIGO-India: Why is it a good idea?… for the World

• Strategic geographical relocation for GW astronomy– sky coverage gain– distance:– duty cycle:

• Potentially large science community in future– Indian demographics: youth dominated – need challenges– excellent UG education system already produces large number of trained

in India find frontline research opportunity at home.

• Large data analysis trained manpower and facilities exist (and being created.

LIGO-India: … the opportunity

Strategic Geographical relocation

Network: HIJLV  GMRT BangaloreMean horizon distance: 1.57 1.63Detection Volume: 12.0 12.0Volume Filling factor: 73% 66%Triple Detection Rate(80%):  8.62 8.64Triple Detection Rate(95%):  11.1 11.1Sky Coverage:  100% 100%Directional Precision:  2.93 3.00

Figure?

LIGO-India: … the opportunity

Strategic Geographical relocation

Source localization error

5-15 degrees to ~degree !!!

Ellipses version as in LIGO-Aus proposal ?

LIGO-India: … the opportunityStrategic Geographical relocation

Polarization info

Sky coverage ?

LIGO-India: … the opportunity

Strategic Geographical relocation- the science gain

Sky coverage: Synthesized Network beam(antenna power)

LIGO-India: … the opportunity

Strategic Geographical relocation- the science gain

Sky coverage: ‘reach’ /sensitivity in different directions

LIGO-India: the concept …• LIGO Lab approached with concept proposal for

joint mega-project --- strategic geographical relocation of

• Advanced LIGO interferometer detector funded and ready to be shipped by US

• Indian contribution in infrastructure : site vacuum systemRelated ControlsData centre trained manpower for installation,

commissioning and running for 10 years

The Science Payoffs• New Astronomy, New Astrophysics, New Cosmology, New

Physics…A New Window ushers a New Era of Exploration• Testing Einstein’s GR in strong and time-varying fields• Testing Black Hole phenomena• Understanding nuclear matter by Neutron star EOS• Neutron star coalescence events• Understanding most energetic events in the

universe..Supernovae, Gamma-ray bursts, LMXB’s, Magnetars• New cosmology..SMBHB’s as standard sirens..EOS of Dark

Energy• Multi-messenger astronomy• The Unexpected

The Technology Payoffs• Lasers and optics..Purest laser light..Low phase noise,

excellent beam quality, high single frequency power• Applications in precision metrology, medicine, micro-

machining• Coherent laser radar and strain sensors for earthquake

prediction and other precision metrology• Surface accuracy of mirrors 100 times better than telescope

mirrors..Ultra-high reflective coatings• Vibration Isolation and suspension..Applications for moneral

prospecting• Squeezing and quantum limits• Ultra-high vacuum system 10^-9 torr..Largest in the region• Computation Challenges

LIGO-India: … the Opportunity

• Part of a fundamental scientific discovery : direct detection of gravitational radiation

• Part of “historic” launch of a new window of Astronomy• LIGO-India: Southernmost, hence, Unique role in the

Intl. GW observatory network.

• Full detector at about half the cost is the naïve calculation.

Adv. LIGO detector system is worth 15 years of challenging R &D – price tag?

• Indian Labs & Industry • •

LIGO-India

LIGO-India: … the opportunityLIGO-India : Technology gain

• 180 W pre-stablized Nd:YAG laser

• Input condition optics, including electro-optic modulators, Faraday isolators, a suspended mode-cleaner (12-m long mode-defining cavity), and suspended mode-matching telescope optics.

• five "BSC chamber" seismic isolation systems (two stage, six degree of freedom, active isolation stages capable of ~200 kg payloads)

• six "HAM Chamber" seismic isolation systems (one stage, six degree of freedom, active isolation stages capable of ~200 kg payloads)

• eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation

• 10 interferometer core optics (test masses, folding mirrors, beam splitter, recycling mirrors)

Relative valuation ?

LIGO-India: … the opportunityLIGO-India : Technology gain

* Five quadruple stage large optics suspensions systems

* Triple stage suspensions for remaining suspended optics

* Baffles and beam dumps for controlling scattering and stray radiation

* Optical distortion monitors and thermal control/compensation system for large optics

* Photo-detectors, conditioning electronics, actuation electronics and conditioning

* Data conditioning and acquisition system, software for data acquisition

* Supervisory control and monitoring system, software for all control systems

* Installation tooling and fixturing

Relative valuation ?

LIGO-India: … the challenges Organizational

National level mega-project Identify a lead institution and agency Project leaderTrain manpower for installation & commissioning Generate & sustain manpower running for 10 years. Site short lead time International competetion

Technical vacuum system Related Controls Data centre

LIGO-India: … the challenges

Trained Manpower for installation & commissioning

Requirements:From LIGO requirements doc

Plans & Preliminary exploration:

NEED TO CONVERGE WITH UNNI AND EXPTERS

Collate and finalizeSendhil doc

LIGO-India: … the challenges

Generate manpower for sustenance of the Intl. observatory

Requirements:

Plans & Preliminary exploration:

• Summer internships in Intl labs underway• IndIGO schools

Proposals:Post graduate school specialization course

LIGO-India: … the challengesLarge scale ultra-high Vacuum enclosure

Requirements:

Preliminary exploration:

LIGO-India: … the challengesIndian SiteRequirements:

Low seismicityLow human generated noiseAir connectivity, Acad institution, labs, industry

Preliminary exploration: IISc new campus & adjoining campuses near Chitra Durga

• 1hr from Intl airport• low seismicity• National science facilities complex plans• •

LIGO-India: … the challengesShort lead time

Requirements:

Preliminary exploration:

LIGO-India: … the challengesInternational competition

Issues:

Preliminary assessment:

Summary (& next steps?)• Of all the large scientific projects out there, this one is

pushing the greatest number of technologies the hardest. • Every single technology they’re touching they’re pushing,

and there’s a lot of different technologies they’re touching. (Beverly Berger, National Science Foundation Program director for gravitational physics. )

• One is left speculating if by the centenary of General Relativity in 2015, the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of general relativity.

THE END

Future GWDA Plans of IndIGO (as part of LSC)

Project leads: Sanjit Mitra, T. Souradeep, S. Dhurandhar …

Extend GW radiometer work (Mitra,Dhurandhar, TS,…2009) Implementation of the cross-correlation search for

periodic sources (Dhurandhar + collab.)

Burst Sources • Formulation• Implementation

Courtesy: S. Dhurandhar

Vetoes for non-Gaussian noise for coherent detection of inspirals

• Project leads: Anand Sengupta, Archana Pai, M K Harris.

Non-Gaussian noise plagues the detector data

Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case

For coincidence search the veto is obvious but for coherent not so.

Developing a veto for coherent is crucial – chi squared

Scope for improving the current chi squared test – Japanese collaboration

8th February Delhi Courtesy: S. Dhurandhar

Tests of General Relativity using GW observations

Project leads:   K G Arun, Rajesh Nayak and Chandra Kant Mishra, Bala Iyer

GWs are unique probes of strong field gravity. Their direct detection would enable very precise tests of GR in the dynamical and strong field regime.

Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC.

Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods.

Possible collaboration with B S Sathyaprakash (Cardiff University) & P Ajith (Caltech).

Courtesy: S. Dhurandhar

Indo-Aus.Meeting, Delhi, Feb 2011

Detector subsystem leaders: approximately 10 talented scientists or researchengineers with interest and knowledge collectively spanning: Lasers and optical devices Optical metrology, handling and cleaning Precision mechanical structures Low noise electronics Digital control systems and electro-mechanical servo design Vacuum cleaning and handling

We will easily be able to find, train and commit people in 4 areas:lasers and optical devices, optical metrology, low noise electronics,digital control and electro-mechanical servo design

Precision mechanical structures and vaccuum systems is also possible,but I would have to talk to other faculty.

I say find, train and commit, because we don't have too manyscientific staff in the institute. The modus operandi would be tostart off with project staff, who are working towards a degree andhence are committed for 3-4 years, and who can then be absorbed intoLIGO-India. An alternative way is to sponsor the degree directly (wejust started a program for Texas Instr, where students get a 50%higher stipend, work only on TI projects, and are guaranteed jobs atTI). Numbers won't be a problem, if there is demand. Our presentannual intake in optics is around 15, so identifying 3-5 is easyenough. We always have tons of applicants for our programs, butquality is a bit spotty, so training becomes important.

The higher level positions at project system engineer, detector leaderand project engineering staff, should be hired for pay, comparable toany large engineering project. People are there.....it is just thatsomeone like HCL or GE, forks out 8-10 lakhs/year for one of our freshMaster's students. So, if LIGO-India pays, they will join.

Change in Length manifests as Change in Transmitted Light

GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins.

Laser Interferometer GW Observatory

4 km: 1.2m diameter high vaccum tubesIndia

180 W(Germany)

Seismic isolation

Stacks (GEO, U

K)

Optics & controls(USA)

40 kgFused silica

mirrors(USA)

Fig from LIGO-AUS report?

If retained get better res picture

Era of Advanced LIGO detectors: 2015