1. An Indo-US joint mega-project concept proposal
LIGO-India Detecting 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: BRI Jun 10, 2011

2. Space Time as a fabric
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.

3. Space Time as a fabric

4. beautiful & successful theory of modern physics.
Einstein’s General theory of relativity
is the most
beautiful & successful
theory of modern physics.
It has matched all tests of Gravitation remarkably well.

5. What happens when matter is in motion?

6. Space-time ripples or gravitational waves
Einstein’s theory predicts
Matter in motion fluctuation in the curvature of space-time which propogates as a wave
Space-time ripples or gravitational waves

7. Binary Neutron stars
Pulsar
companion

8. GW from Binary Neutron stars

9. Indirect evidence for Gravity waves
Won the Nobel prize
in 1993 !!!
Binary pulsar emits gravitational waves
leads to loss of orbital energy
period speeds up 14 sec from
measured to ~50 msec accuracy
deviation grows quadratically with time
Hulse and Taylor
Results for PSR

10. Effect of GW on test masses

11. Effect of GW on a ring of test masses
Interferometer mirrors as test masses

12. Detecting GW with Laser InterferometerB A
Path A
Path B
Difference in distance of Path A & B  Interference of laser light at the detector (Photodiode)

13. Path difference  phase difference
Equal arms: Dark fringe
The effects of gravitational waves appear as a fluctuation in the phase differences between two orthogonal light paths of an interferometer.
Unequal arm:
Signal in PD

14. Challenge of Direct Detection
Gravitational waves are very weak!
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!

15. GW Astronomy with Intl. Network of GW Observatories
1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info.
LIGO-LLO: 4km
LIGO-LHO: 2km, 4km
GEO: 0.6km
VIRGO: 3km
TAMA: 0.3km
LIGO-Australia?
LCGT??
LIGO-India ?

16. A Century of Waiting
Almost 100 years since GW were theoretically predicted By Albert Einstein but still no direct experimental confirmation a la Hertz
Reason is connected to two fundamental differences between EM and
Gravitation:
- The weakness of the gravitational interaction relative to EM (10􀀀39)
-The spin two nature of gravitation compared to the spin one nature
of EM that forbids dipole radiation in GR.
Implies low efficiency for conversion of mechanical energy to gravitational radiation. And feeble effects of GW on any potential detector.
A GW Hertz experiment is ruled out and it is only signals produced by astrophysical systems where there are potentially huge masses accelerating very strongly that are likely sources.

17. Gravitational Waves Exist!
High quality data which is proof that GW exist.
In 1974 Hulse and Taylor, discovered the Binary Pulsar
The system has now been monitored for 30 years. Orbital period slowly decreasing at just the rate predicted by GR for emission of GW!!!
Hulse and Taylor received Nobel Prize for this (1993).
ADD FIGURES

18. Laser Interferometric Gravitational Wave Detectors?
Binary Pulsars establish Reality of Grav Radn. Validity of GR in Strong Fields. Excellent Evidence but Evidence is Indirect
Can detectors be built to attempt a Direct detection of these GW??
GW are transverse and tidally distort a system in directions
perpendicular to propagation direction.
Effect measured by the Dimensionless strain h = 2( Delta L)/ L, it produces
For a typical NS binary in Virgo cluster (18 Mpc; 5.6 x 10^20 km)
h = 4G/ c^4 Knonsph/D ~ (2 GM/ Rc^2) (GM/Dc^2) ~ 1.5 x 10^-21
The miniscule strain and associated tiny displacement must be
measured to detect the GW.
Weber's Bar detectors (Narrow band);
Today's Laser Interferometric Detectors ( Broad Band)
As a GW passes, the arm lengths of km scale ITF change (10^-18m)
tidally causing the interference pattern to change at the photodiode
Direct detection of GW -
First mandate of Laser Interferometric GW detectors
Promised and Real Excitement - New Observational Window and
Tool for Astrophysics; Experimental Probe for Basic Physics

19. 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.

21. LIGO and Virgo TODAY
Field 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..

22. Expected Annual Coalescence Rates
In a 95% condence interval, rates uncertain by 3 orders of magnitude
NS-NS ( ); NS-BH ( ) ; BH-BH ( ) yr^-1
Based on Extrapolations from observed Binary Pulsars,Stellar birth rate
estimates, Population Synthesis models. Rates quoted below are mean of the distribution.
Detector Generation
NS-NS
NS-BH
BH-BH
Initial LIGO
( )
0.02
0.0006
0.0009
Enhanced LIGO
(2X Sensitivity)
( )
0.1
0.04
0.07
Advanced LIGO
(10X sensitivity)
( …) 40
10.
20.0

23. Laser Interferometer GW Observatory
40 kg
Fused silica
mirrors
(USA)
Seismic isolation
Stacks (GEO, UK)
Optics & controls
(USA)
4 km: 1.2m diameter high vaccum tubes
India
Fig from LIGO-AUS report?
180 W
(Germany)

24. Schematic Optical Design of Advanced LIGO detectors

25. Era of Advanced LIGO detectors: 2015
If retained get better res picture

26. 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,…
Courtesy: B. Schutz, GWIC Roadmap Document 2010

27. INDIGO: the goals LIGO-India (Letter from LIGO Labs)
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,…

28. Multi-disciplinary Consortium
Multi-Institutional,
Multi-disciplinary Consortium
CMI, Chennai
Delhi University
IISER Kolkata
IISER Trivandrum
IIT Madras
IIT Kanpur
IUCAA
RRCAT
TIFR
RRI
IPR, Bhatt
Jamia Milia Islamia
Tezpur Univ

29. Instrumentation & Experiment
The IndIGO Consortium
IndIGO Council
Bala Iyer ( Chair) RRI, Bangalore
Sanjeev Dhurandhar (Science) IUCAA, Pune
C. S. Unnikrishnan (Experiment) TIFR, Mumbai
Tarun Souradeep (Spokesperson) IUCAA, Pune
Data Analysis & Theory
Sanjeev Dhurandhar IUCAA
Bala Iyer RRI
Tarun Souradeep IUCAA
Anand Sengupta Delhi University
Archana Pai IISER, Thiruvananthapuram
Sanjit Mitra JPL , IUCAA
K G Arun Chennai Math. Inst., Chennai
Rajesh Nayak IISER, Kolkata
A. Gopakumar TIFR, Mumbai
T R Seshadri Delhi University
Patrick Dasgupta Delhi University
Sanjay Jhingan Jamila Milia Islamia, Delhi
L. Sriramkumar, Phys., IIT M
Bhim P. Sarma Tezpur Univ .
P Ajith Caltech , USA
Sukanta Bose, Wash. U., USA
B. S. Sathyaprakash Cardiff University, UK
Soumya Mohanty UTB, Brownsville , USA
Badri Krishnan Max Planck AEI, Germany
Instrumentation & Experiment
C. S. Unnikrishnan TIFR, Mumbai
G Rajalakshmi TIFR, Mumbai
P.K. Gupta RRCAT, Indore
Sendhil Raja RRCAT, Indore
S.K. Shukla RRCAT, Indore
Raja Rao ex RRCAT, Consultant
Anil Prabhakar, EE, IIT M
Pradeep Kumar, EE, IIT K
Ajai Kumar IPR, Bhatt
S.K. Bhatt IPR, Bhatt
Ranjan Gupta IUCAA, Pune
Rijuparna Chakraborty, Cote d’Azur, Grasse
Rana Adhikari Caltech, USA
Suresh Doravari Caltech, USA
Biplab Bhawal (ex LIGO)

30. IndIGO Advisory Structure
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)
Program Management committee
C S Unnikrishnan (TIFR, Mumbai), Chair.
Bala R Iyer (RRI, Bangalore), Coordinator
Sanjeev Dhurandhar (IUCAA, Pune) Co-cordinator
Tarun 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

31. 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.

32. 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.

33. GWIC: Gravitational Wave International Committee
Courtesy: B. Schutz: GWIC Roadmap Document

34. Indo-Aus.Meeting, Delhi, Feb 2011

35. 23 July 2011
Dear 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……

36. 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 system
Related Controls
Data centre
trained manpower for installation, commissioning and running for 10 years

37. The Science payoffs
New Physics, New Astronomy, New Astrophysics, New Cosmology..
A New Window ushers a new era of exploration..
Testing Einstein's GR..
Black hole phenomena..
Understanding nuclear matter by neutron star EOS
Neutron star coalescence events
Listening to most energetic events in the universe.
Supernovae, Gamma ray bursts, Magnetars
New Cosmology: Standard Sirens..Determine EOS of Dark energy
Multi-messenger Astronomy
The Unexpected!!

38. 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.
Ultrahigh reflective coatings..
Vibration isolation and suspension..Applications for mineral
prospecting
Sqeezing and QM limits
Ultra high vacuum system 10^-9 torr..
Largest in this region
Computation Challenges f

42. 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

43. Strategic Geographical relocation
LIGO-India: … the opportunity
Strategic Geographical relocation
- the science gain
Sky coverage
: Synthesized
Network
beam
(antenna power)

44. Strategic Geographical relocation
LIGO-India: … the opportunity
Strategic Geographical relocation
- the science gain
Sky coverage: ‘reach’ /sensitivity in different directions

45. Strategic Geographical relocation
LIGO-India: … the opportunity
Strategic Geographical relocation
Source localization error
5-15 degrees to ~degree !!!
Ellipses version as in LIGO-Aus proposal ?

46. Strategic Geographical relocation
LIGO-India: … the opportunity
Strategic Geographical relocation
Polarization info
Sky coverage ?

53. Strategic Geographical relocation
LIGO-India: … the opportunity
Strategic Geographical relocation
Figure?
Network: HIJLV  GMRT Bangalore
Mean horizon distance:
Detection Volume:
Volume Filling factor: 73% 66%
Triple Detection Rate(80%): 
Triple Detection Rate(95%): 
Sky Coverage:  % 100%
Directional Precision: 

54. LIGO-India : Technology gain
LIGO-India: … the opportunity
LIGO-India : Technology gain
Relative valuation ?
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)

55. LIGO-India : Technology gain
LIGO-India: … the opportunity
LIGO-India : Technology gain
Relative valuation ?
* 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

56. 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.

57. LIGO-India: … the challenges Organizational
National level mega-project
Identify a lead institution and agency
Project leader
Train manpower for installation & commissioning
Generate & sustain manpower running for 10 years.
Site
short lead time
International competetion
Technical
vacuum system
Related Controls
Data centre

58. LIGO-India: … the challenges
Trained Manpower for installation & commissioning
Requirements:
From LIGO requirements doc
Plans & Preliminary exploration:
Sendhil doc

59. Indo-US centre for Gravitational Physics and Astronomy
APPROVED for funding (Dec 2010)
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

60. 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

61. Large scale ultra-high Vacuum enclosure
LIGO-India: … the challenges
Large scale ultra-high Vacuum enclosure
Requirements:
Preliminary exploration:

62. Indian Site LIGO-India: … the challenges Requirements: Low seismicity
Low human generated noise
Air 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

63. Short lead time LIGO-India: … the challenges Requirements:
Preliminary exploration:

64. Internation competition
LIGO-India: … the challenges
Internation competition
Issues:
Preliminary assessment:

65. LIGO-India

66. 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!!
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.

67. 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

68. Objectives of the data centre
Tier 2
Data Centre
at IUCAA
Archival
Community
development
Indian Researchers and Students
TIER3 centres at
Univ & IISERS
Other science groups
Web Services
Collaboration tools
Analysis
LSC
LIGO Data Grid
LIGO Data Grid as a role model for the proposed
IndIGO Data Analysis Centre.
Courtesy: Anand Sengupta

69. IndIGO Data Centre@IUCAA Indian Initiative in Gravitational-wave Observations
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/core
Need 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

70. 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

71. 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

72. 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

73. Summary (& next steps?)

74. THE END

75. 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.

76. Indo-Aus.Meeting, Delhi, Feb 2011