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: 4 Jun 14, BRI

2. Space Time as a fabric Matter tells space-time how to curve, and
Special Relativity (SR) replaced Absolute space and Absolute Time by flat 4-dimensional space-time (the normal three dimensions of space, plus a fourth dimension of time).
In 1916, Albert Einstein published his famous Theory of General Relativity, his theory of gravitation consistent with SR, where gravity manifests as a curved 4-diml space-time
Theory describes how space-time is affected by mass and also how energy, momentum and stresses affects space-time.
Matter tells space-time how to curve, and
Space-time tells matter how to move.

3. Space Time as a fabric
Earth follows a straight line in the curved space-time caused by sun’s mass !!!

4. beautiful, as well as, successful Era of precision tests : GP-B,….
Beauty & Precision
Einstein’s General theory of relativity is the most
beautiful, as well as, successful
theory of modern physics.
It has matched all experimental tests of Gravitation remarkably well.
Era of precision tests : GP-B,….

5. What happens when
matter is in motion?

6. Einstein’s Gravity predicts
Matter in motion Space-time ripples fluctuations in space-time curvature that propagate as waves
Gravitational waves (GW)
In GR, as in EM, GW travel at the speed of light (i.e., mass-less) , are transverse and have two states of polarization.
The major qualitatively unique prediction beyond Newton’s gravity
Begs direct verification !!!

7. 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 experiment ruled out. Only astrophysical systems involving huge masses and accelerating very strongly are potential sources of GW signals.

8. Energy emitted in GW from binary >> EM radiation in the lifetime
GW  Astronomy link
Astrophysical systems are sources of copious GW emission:
Typically, GW emission (0.1) >> EM radiation via Nuclear process (0.025)
Energy emitted in GW from binary >> EM radiation in the lifetime
Universe is buzzing with GW signals from cores of astrophysical events
Bursts (SN, GRB), mergers, accretion, stellar cannibalism ,…
Extremely Weak interaction, hence, has been difficult to detect directly
But also implies GW carry unscreened & uncontaminated signals

9. GW from Binary Neutron stars
Pulsar
companion

10. Nobel prize in 1993 !!! Indirect evidence for Gravity waves
Binary pulsar systems emit 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

11. Principle behind Detection of GW

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

13. 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)

14. Equal arms: Dark fringe
Interferometry
Path difference of light
 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

15. one part in thousand-billion-billion!
Challenge of Direct Detection
Gravitational wave is measured in terms of strain, h
(change in length/original length)
Gravitational waves are very weak!
Expected amplitude of GW signals
Measure changes of
one part in thousand-billion-billion!

16. LIGO Optical Configuration
Michelson
Interferometer
Light is “recycled” about 50 times
Power Recycled
end test mass
beam splitter
signal
with Fabry-Perot Arm Cavities
Light bounces back and forth along arms about 100 times
input test mass
Laser
Courtesy: Stan Whitcomb

17. Initial LIGO Sensitivity Goal
Strain sensitivity <3x /Hz1/2 at 200 Hz
Sensor Noise
Photon Shot Noise
Residual Gas
Displacement Noise
Seismic motion
Thermal Noise
Radiation Pressure

18. LIGO and Virgo TODAY
Milestone: Decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwide
Experimental prowess: LIGO, VIRGO operating at predicted sensitivity!!!!
Pre-dawn GW astronomy : Unprecedented sensitivity already allows
Upper Limits on GW from a variety of Astrophysical sources. Refining theretical modelling
Improve on Spin down of Crab, Vela pulsars,
Exptally surpass Big Bang nucleosynthesis bound on Stochastic GW..

19. Laser Interferometer Gravitational-wave Observatory (LIGO)
IndIGO - ACIGA meeting

20. Astrophysical Sources for Terrestrial GW Detectors
Compact binary inspiral: “chirps”
NS-NS, NS-BH, BH-BH
Supernovas or GRBs: “bursts”
GW signals observed in coincidence with EM or neutrino detectors
Pulsars in our galaxy: “periodic waves”
Rapidly rotating neutron stars
Modes of NS vibration
Cosmological: “stochastic background” ?
Probe back to the Planck time (10-43 s)
Probe phase transitions : window to force unification
Cosmological distribution of Primordial black holes
Courtesy;: Stan Whitcomb

21. Using GWs to Learn about the Source an Example
Over two decades, RRI involved in computation of inspiral waveforms for compact binaries & their implications and
IUCAA in its Data Analysis Aspects.
Can determine
Distance from the earth r
Masses of the two bodies
Orbital eccentricity e and orbital inclination i

22. Advanced LIGO Take advantage of new technologies and on-going R&D
>> Active anti-seismic system operating to lower frequencies:
(Hannover, GEO)
>> Lower thermal noise suspensions and optics :
(GEO )
>> Higher laser power 10 W  180 W
(Hannover group, Germany)
>> More sensitive and more flexible optical configuration:
Signal recycling (GEO)
Design: 1999 – 2010 : 10 years of high end R & D internationally.
Construction: Start 2008; Installation 2011; Completion 2015

23. “Quantum measurements” to improve further via squeezed light:
A big draw for the large Indian theoretical physics community & students !!!
(& of course, optics technology)

24. Tailoring the frequency response
Signal Recycling : New idea in interferometry
Additional cavity formed with mirror at output
Can be made resonant, or anti-resonant, for gravitational wave frequencies
Allows redesigning the noise curve
to create optimal band sensitive to specific astrophysical signatures

25. Schematic Optical Design of Advanced LIGO detectors
Reflects International cooperation
Basic nature of GW Astronomy
LASER
AEI, Hannover
Germany
Seismic isolation Suspension
GEO, UK

26. Courtesy: Stan Whitcomb
Advanced LIGO Laser
Designed and contributed by Albert Einstein Institute< Germany
Higher power
10W -> 180W
Better stability
10x improvement in intensity and frequency stability
Courtesy: Stan Whitcomb

27. Courtesy: Stan Whitcomb
Advanced LIGO Mirrors
Larger size
11 kg -> 40 kg
Smaller figure error
0.7 nm -> 0.35 nm
Lower absorption
2 ppm -> 0.5 ppm
Lower coating thermal noise
All substrates delivered
Polishing underway
Reflective Coating process starting up
Courtesy: Stan Whitcomb

28. Advanced LIGO Seismic Isolation
Two-stage six-degree-of-freedom active isolation
Low noise sensors, Low noise actuators
Digital control system to blend outputs of multiple sensors, tailor loop for maximum performance
Low frequency cut-off: 40 Hz -> 10 Hz
Courtesy: Stan Whitcomb

29. Advanced LIGO Suspensions
UK designed and contributed test mass suspensions
Silicate bonds create quasi-monolithic pendulums using ultra-low loss fused silica fibres to suspend interferometer optics
Pendulum
Q ~105 -> ~108
Suppression at 10 Hz : ?
at 1 Hz : ?
40 kg silica test mass
four stages 29
Courtesy: Stan Whitcomb

30. nearest super-clusters) A Day of Advanced LIGO Observation >>
Era of Advanced LIGO detectors: 2015
10x sensitivity
10x reach
1000 volume
>> 1000 event rate
(reach beyond
nearest super-clusters)
A Day of Advanced LIGO Observation >>
A year of Initial LIGO

31. Expected Annual Coalescence Event Rates
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
In a 95% confidence 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.

32. Advanced GW network sensitivity needed to observe
Scientific Payoffs
Advanced GW network sensitivity needed to observe
GW signals at monthly or even weekly rates.
Direct detection of GW probes strong field regime of gravitation
 Information about systems in which strong-field and time dependent gravitation dominates, an untested regime including non-linear self-interactions
GW detectors will uncover NEW aspects of the physics
 Sources at extreme physical conditions (eg., super nuclear density physics), relativistic motions, extreme high density, temperature and magnetic fields.
GW signals propagate un-attenuated
weak but clean signal from cores of astrophysical event where EM signal is screened by ionized matter.
Wide range of frequencies  Sensitivity over a range of astrophysical scales
To capitalize one needs a global array of GW antennas separated by continental distances to pinpoint sources in the sky and extract all the source information encoded in the GW signals

33. 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
LCGT 4km
TAMA/CLIO
LIGO-Australia?
LIGO-India ?

34. From the GWIC Strategic Roadmap for GW Science with thirty year horizon (2007)
… the first priority for ground-based gravitational wave detector development is to expand the network, adding further detectors with appropriately chosen intercontinental baselines and orientations to maximize the ability to extract source information. ….Possibilities for a detector in India (IndIGO) are being studied..

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

36. Synergy with other major Astronomy projects
Gravitational wave Astronomy :
vit
Synergy with other major Astronomy projects
SKA -Radio : Pulsars timing,
X-ray satellite (AstroSat) : High energy physics
Gamma ray observatory:
Thirty Meter Telescope: Resolving multiple AGNs, gamma ray follow-up after GW trigger,…
LSST: Astro-transients with GW triggers.
INO: neutrino signals
Courtesy: B. Schutz, GWIC Roadmap Document 2010

37. The Gravitational wave legacy
Two decades of Indian contribution to the international effort for detecting GW on two significant fronts :
Seminal contributions to source modeling at RRI [Bala Iyer] and to GW data analysis at IUCAA [Sanjeev Dhurandhar] which has been internationally recognized
RRI: Indo-French collaboration for two decades to compute high accuracy waveforms for in-spiraling compact binaries from which the GW templates used in LIGO and Virgo are constructed.
IUCAA: Designing efficient data analysis algorithms involving advanced mathematical concepts.
Notable contributions include the search for binary in-spirals, hierarchical methods, coherent search with a network of detectors and the radiometric search for stochastic gravitational waves.
IUCAA has collaborated with most international GW detector groups and has been a member of the LIGO Scientific Collaboration.
At IUCAA, Tarun Souradeep with expertise in CMB data and Planck has worked to create a bridge between CMB and GW data analysis challenges.

38. Indian Gravitational wave strengths
Very good students and post-docs produced from these activities.
* Leaders in GW research abroad [Sathyaprakash, Bose, Mohanty] (3) *Recently returned to faculty positions at premier Indian institutions (6) [Gopakumar, Archana Pai, Rajesh Nayak, Anand Sengupta, K.G. Arun, Sanjit Mitra, P. Ajith?]
Gopakumar (?) and Arun (?) : PN modeling, dynamics of CB, Ap and cosmological implications of parameter estimation
Rajesh Nayak (UTB  IISER K) , Archana Pai (AEI  IISER T), Anand Sengupta (LIGO, Caltech Delhi), Sanjit Mitra (JPL  IUCAA ): Extensive experience on single and multi-detector detection, hierarchical techniques, noise characterisation schemes, veto techniques for GW transients, bursts, continuous and stochastic sources, radiometric methods, …
P. Ajith (Caltech, TAPIR  ? ) ……
Sukanta Bose (Faculty UW, USA  ?)
Strong Indian presences in GW Astronomy with Global detector network  broad international collaboration is the norm  relatively easy to get people back.
Close interactions with Rana Adhikari (Caltech), B.S. Sathyaprakash (Cardiff), Sukanta Bose ( WU, Pullman), Soumya Mohanty (UTB), Badri Krishnan ( AEI) …
Very supportive Intl community reflected in Intl Advisory somm of IndIGO

39. High precision and Large experiment in India
C.S. Unnikrishnan (TIFR) : involved in high precision experiments and tests
Test gravitation using most sensitive torsional balances and optical sensors.
Techniques related to precision laser spectroscopy, electronic locking, stabilization.
Ex students from this activity G.Rajalakshmi (TIFR, 3m prototype) Suresh Doravari (Caltech 40m)
Groups at BARC and RRCAT : involved in LHC
providing a variety of components and subsystems like precision magnet positioning stand jacks, superconducting correcting magnets, quench heater protection supplies and skilled manpower support for magnetic tests and measurement and help in commissioning LHC subsystems.
S.K. Shukla at RRCAT on INDUS: UHV experience.
S.B. Bhatt and Ajai Kumar at IPR on Aditya: UHV experience.
A.S. Raja Rao (ex RRCAT) : consultant on UHV
Sendhil Raja (RRCAT) :
Optical system design
laser based instrumentation, optical metrology
Large aperture optics, diffractive optics, micro-optic system design.
Anil Prabhakar IITM and Pradeep Kumar IITK (EE dept s)
Photonics, Fiber optics and communications
Characterization and testing of optical components and instruments for use in India..
Rijuparna Chakraborty (Observatoire de la Cote d'Azur)..Adaptive Optics..
Under consideration for postdoc in LIGO or Virgo….

40. Multi-disciplinary Consortium (2009)
Multi-Institutional,
Multi-disciplinary Consortium
(2009)
CMI, Chennai
Delhi University
IISER Kolkata
IISER Trivandrum
IIT Madras (EE)
IIT Kanpur (EE)
IUCAA
RRCAT
TIFR
RRI
IPR, Bhatt
Jamia Milia Islamia
Tezpur Univ

41. 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)

42. 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……

43. 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)]

44. The Science & technology benefit of LIGO-India is transformational
IndIGO: the goals
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 - Sendhil Raja, Anil Prabhakar, Pradeep Kumar
Ultra High Vacuum & controls at RRCAT, IPR, BARC, ISRO, …. Shukla, Raja Rao, Bhatt,
UG summer internship at National & International GW labs & observatories.
Postgraduate IndIGO schools, specialized courses,…
Consolidated IndIGO membership of LIGO Scientific Collaboration in Advanced LIGO
Proposal to create a Tier-2 data centre for LIGO Scientific Collaboration in IUCAA
IUSSTF Indo-US joint Centre at IUCAA with Caltech (funded)
Major experimental science initiative in GW astronomy
Earlier Plan: Partner 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.
Today: 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 arm length high vacuum tubes in L configuration
Indian cost ~ Rs 1000Cr
The Science & technology benefit of LIGO-India is transformational

45. IndIGO Data Centre@IUCAA
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
Large University sector participation via IUCAA
200 Tflops peak capability
Storage: 4x100TB per year per interferometer.
Network: gigabit+ backbone, National Knowledge Network
Gigabit dedicatedlink to LIGO lab Caltech
Courtesy: Anand Sengupta, IndIGO

46. 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

47. LIGO-India from LIGO Dear Prof. Kasturirangan, 1 June 2011
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 from LIGO
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.

48. 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.

49. LIGO-India: Why is it a good idea? … for the World
Strategic geographical relocation for GW astronomy
Improved duty cycle
Detection confidence
Improved Sky Coverage
Improved Location of Sources required for multi-messenger astronomy
Determine the two polarizations of GW
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.

50. LIGO-India: Salient points (vis a vis other mega-projects)
On Indian Soil
Historical science discovery participation
Expenditure mostly in Indian labs & Industry
International Cooperation, not competition
Shared science risk with Intl. community
Initial setup risks, troubleshooting rests with Advance LIGO USA
Well defined training possibility at advance LIGO USA installation and commissioning for Indian technical team
Related major data analysis centre with huge University secto involvement.

51. Strategic geographical relocation comparison
Network
HHLV
HILV
AHLV
Mean horizon distance
1.74
1.57
1.69
Detection Volume
8.98
8.77
8.93
Volume Filling factor
41.00%
54.00%
44.00%
Triple Detection Rate(80%)
4.86
5.95
6.06
Triple Detection Rate(95%)
7.81
8.13
8.28
Sky Coverage: 81%
47.30%
79.00%
53.50%
Directional Precision
0.66
2.02
3.01

52. 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 ?

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

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

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

57. LIGO-Lab contribution to LIGO-India
LIGO-India: unique once-in-a-generation opportunity
LIGO-Lab contribution to LIGO-India
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)

58. LIGO-Lab contribution to LIGO-India
LIGO-India: unique once-in-a-generation opportunity
LIGO-Lab contribution to LIGO-India
* 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

59. LIGO-India: Indian Contributions
Indian contribution in infrastructure :
Site
Vacuum system
Related Controls
Data centre
Trained manpower for installation and commissioning
Trained manpower for LIGO-India operations for 10 years

60. LIGO-India vs future IndianIGO : Major Advantages
Cutting edge instrument to jump start GW astronomy. Would require at least a decade of focused technology development to get there
180 W Nd-Yag: 5 years; Rs crores. Operation and maintenance should benefit further development in narrow line width lasers. Applications in high resolution spectroscopy, precision interferometry and metrology.
Input condition optics..Expensive..No Indian manufacturer with such specs
BSC, HAM.. Minimum 2 of years of experimentation and R&D. Experience in setting up and maintaining these systems  know how for isolation in critical experiments such as in optical metrology, AFM/Microscopy, gravity experiments etc.
10 interferometer core optics.. manufacturing optics of this quality and develop required metrology facility : At least 5 to 7 years of dedicated R&D work in optical polishing, figuring and metrology.
Five quadruple stage large optics suspensions systems years of development.. Not trivial to implement. Benefit other physics experiments working at the quantum limit of noise.

61. 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

62. 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 mineral prospecting
Squeezing and quantum limits
Ultra-high vacuum system 10^-9 torr..Largest in the region
Computation Challenges; Cloud computing, new hardware and software tools for computational innovation

63. The rewards and spinoffs
Detection of GW is the very epitome of breakthrough science.
In collaborating with USA to realize LIGO-India, India could become a partner in international science of Nobel Prize significance
GW detection is an instrument technology intensive field pushing frontiers simultaneously in a number of fields like lasers and photonics. Impact allied areas and smart industries.
The imperative need to work closely with industry and other end users will lead to spinoffs as GW scientists further develop optical sensor technology.
Presence of LIGO-India will lead to pushing technologies and greater innovation in the future.
The largest UHV system will provide industry a challenge and experience.

64. …The rewards and spinoffs
LIGO-India can raise profile of science since it will be making ongoing discoveries fascinating the young. GR, BH, EU and Einstein has a special attraction and a pioneering facility in India participating in important discoveries will provide role models with high visibility and media interest.
LIGO has a strong outreach tradition and LIGO-India will provide a platform to increase it and synergically benefit.
Increase number of research groups performing at world class levels and produce skilled researchers.
Increase number of businesses investing in R&D. Provide opportunities to increase proportion of industries engaging in innovation.
Increase international collaborations in Indian research. Science Leadership in the Asia-Pacific(?) region

65. LIGO-India: … the challenges Organizational
National level DST-DAE Consortium Flagship Mega-project
Identify a lead institution and agency
Project leader
Construction: Substantial Engg project building Indian capability in large vacuum system engg, welding techniques and technology
Complex Project must be well-coordinated and effectively carried out
in time and meeting the almost zero-tolerance specs
Train manpower for installation & commissioning
Generate & sustain manpower running for 10 years.
Site
short lead time
International competition (LIGO-Argentina ??)
Technical
vacuum system
Related Controls
Data centre

66. LIGO-India: … the challenges
Trained Manpower for installation & commissioning
LIGO-India Director
Project manager
Project engineering staff:
Civil engineer(s)
Vacuum engineer(s)
Systems engineer(s),
Mechanical engineers
Electronics engineers
Software engineers
Detector leader
Project system engineer
Detector subsystem leaders [10 talented scientists or research engineers
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)]

67. Logistics and Work Plan
Assumption: Project taken up by DAE as a National Mega Flagship Project. All the persons mentioned who are currently working in their centers would be mainly in a supervisory role of working on the project during the installation phase and training manpower recruited under the project who would then transition into the operating staff.
Instrument Engineering: No manpower required for design and development activity. For installation and commissioning phase and subsequent operation
Laser ITF: Unnikrishnan, Sendhil Raja, Anil Prabhaker.
TIFR, RRCAT, IITM. 10 Post-doc/Ph.D students. Over 2-3 years.
Spend a year at Advanced LIGO. 6 full time engineers and scientists. If project sanctioned, manpower sanctioned, hirings possible at RRCAT.. TIFR??

68. Large scale ultra-high Vacuum enclosure
S.K. Shukla (RRCAT),A.S. Raja Rao (ex RRCAT),
S. Bhatt (IPR), Ajai Kumar (IPR)
To be fabricated by IndIGO with designs from LIGO. A pumped volume of 10000m3 (10Mega-litres), evacuated to an ultra high vacuum of 10-9 torr.
Spiral welded beam tubes 1.2m in diameter and
20m length.
Butt welding of 20m tubes together to 200m length.
Butt welding of expansion bellows between 200m tubes.
Gate valves of 1m aperture at the 4km tube ends and the middle.
Optics tanks, to house the end mirrors and beam splitter/power and signal recycling optics vacuum pumps.
Gate valves and peripheral vacuum components.
Baking and leak checking

69. Large scale ultra-high Vacuum enclosure
5 Engineers and 5 technicians to oversee the procurement &
fabrication of the vacuum system components and its installation. If the project is taken up by DAE then participation of RRCAT & IPR will be taken up. All vacuum components such as flanges, gate-valves, pumps, residual gas analyzers and leak detectors will be bought. Companies L&T, Fillunger, HindHiVac, Godrej with support from RRCAT, IPR and LIGO Lab.
Preliminary detailed discussions in Feb 2011 with companies
like HHV, Fullinger in consultation with Stan Whitcomb (LIGO),
D. Blair (ACIGA) since this was a major IndIGO deliverable to
LIGO-Australia
Preliminary Costing for LIGO-India

70. Logistics and Work Plan
Clean rooms: Movable tent type clean rooms during welding of the beam tubes and assembly of the system. Final building a clean room with AC and pressurization modules. SAC, ISRO. 1 engineer and 2 technicians to draw specs for the clean room equipments and installation.
Vibration isolation system: 2 engineers (precision mechanical) to install and maintain the system. Sourced from BARC. RED (Reactor Engineering Division of BARC) has a group that works on vibration measurement, analysis and control in reactors and turbo machinery.
Electronic Control System: 4 Engineers to install and maintain the electronics control and data acquisition system. Electronics & Instrumentation Group at BARC (G. P. Shrivastava’s group) and RRCAT. Preliminary training:six months at LIGO. Primary responsibility (installing and running the electronics control and data acquisition system): RRCAT & BARC. Additional activity for LIGO-India can be factored in XII plan if the approvals come in early.

71. Logistics and Work Plan
Understand teams at Electronics & Instrumentation Group at BARC looking for large instrumentation projects in XII plan.
Control software Interface: 2 Engineers (install and maintain the computer software interface, distributed networking and control system). RRCAT and BARC. Computer software interface (part of the data acquisition system) and is the “Human-machine-interface” for the interferometer. For seamless implementation man power to be sourced from teams implementing Electronic Control System.
Site Selection & Civil Constructions: BARC Seismology Division Data reg. seismic noise at various DAE sites to do initial selection of sites and shortlist based on other considerations such as accessibility and remoteness from road traffic etc. DAE: Directorate of Construction, services and Estate Management (DCSEM): Co-ordinate design and construction of the required civil structures required for the ITF. 2 engineers + 3 technicians (design & supervision of constructions at site). Construction contracted to private construction firm under supervision of DCSEM.
42 persons (10 PhD/postdocs, 22 scientists/engineers and 10 technicians)

72. LIGO-India: … the challenges
Manpower generation for sustenance of the LIGO-India observatory : Plans & Preliminary exploration
Since Advanced LIGO will have a lead time, participants will be identified who will be deputed to take part in the commissioning of Advanced LIGO and later bring in the experience to LIGO-India
Successful Summer internships in International labs underway..
Plan to extend to National labs to generate more experimenters
IndIGO schools are planned annually to expose students to emerging opportunities and attract some to join.
Post graduate school specialization course
Jayant Narlikar: Since sophisticated technology is involved IndIGO should like ISRO or BARC training school set up a program where after successful completion of the training, jobs are assured.

73. Indian Site LIGO-India: … the challenges Requirements: Low seismicity
Low human generated noise
Air connectivity,
Proximity to Academic institution, labs, industry
Preliminary exploration:
IISc new campus & adjoining campuses near Chitra Durga
1hr from Intl airport
low seismicity
National science facilities complex plans

74. LIGO-India: Action points
If accepted as a National Flagship Mega Project under the 12th plan then…
Seed Money
Identification of 3-6 project leaders
Detailed Project Proposal
Site identification
1st Staffing Requirement meeting Aug 1-15
2nd Joint Staffing Meeting with LIGO-Lab
Vacuum Task related team and plans

75. Concluding remarks
A century after Einstein predicted them, and after four decades of very innovative and Herculean struggle, We are on the threshold of a new era in GW detection.
First generation detectors like Initial LIGO and Virgo have reached design sensitivity . Have broken new ground in optical sensitivity, pushed technology and proved the technique.
Second generation detectors are starting installation and expected to expand the “Science” by factor of 1000
A worldwide network is starting to come on line and the ground work has been laid for operation as a integrated system.
An unique once-in-a-generation opportunity for India. India could play a key role by hosting LIGO-India.
A compelling Science case, a proven design. Need strong institutional support to bring together capable participants.

76. Concluding remarks
A GREAT opportunity but a very sharp deadline of 31 Mar If we cannot act quickly the possibility will close. Conditions laid out in the Req Doc of LIGO-Lab will need to be ready for LIGO-Lab examination latest by Dec 2011 so that in turn LIGO-Lab can make a case with NSF by Jan 2012.
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.

77. THE END

78. 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

79. 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

83. LIGO-India

88. 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

89. 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

90. 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

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

93. Detector subsystem leaders: approximately 10 talented scientists or research engineers 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 many scientific staff in the institute. The modus operandi would be to start off with project staff, who are working towards a degree and hence are committed for 3-4 years, and who can then be absorbed into LIGO-India. An alternative way is to sponsor the degree directly (we just started a program for Texas Instr, where students get a 50% higher stipend, work only on TI projects, and are guaranteed jobs at TI). Numbers won't be a problem, if there is demand. Our present annual intake in optics is around 15, so identifying 3-5 is easy enough. We always have tons of applicants for our programs, but quality is a bit spotty, so training becomes important. The higher level positions at project system engineer, detector leader and project engineering staff, should be hired for pay, comparable to any large engineering project. People are there.....it is just that someone like HCL or GE, forks out 8-10 lakhs/year for one of our fresh Master's students. So, if LIGO-India pays, they will join.

94. 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.

96. 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)

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

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

100. 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.

101. 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: 

102. 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

103. International competition
LIGO-India: … the challenges
International competition
Issues:
Preliminary assessment:

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