1. IndIGO Indian Initiative in Gravitational-wave Observations Detecting Einstein’s Elusive Waves Opening a New Window to the Universe Inaugurating Gravitational wave Astronomy LIGO-India: An Indo-US joint mega-project concept proposal IndIGO Consortium Version: pI_v3 Jun 21, 2011 : BI www.gw-indigo.org

2. What are Gravitational waves and how best to detect them??

3. Beauty & Precision

4. 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, are transverse and have two states of polarization. A major qualitatively unique prediction beyond Newton’s gravitation

5. leads to loss of orbital energy period speeds up 14 sec from 1975-94 Pulsar Timing measured to ~50 msec accuracy deviation grows quadratically with time Binary pulsar systems emit gravitational waves Hulse and Taylor Results for PSR1913+16 Indirect evidence for Gravitational waves Nobel prize in 1993 !!! Pulsar companion

6. Courtesy;: Stan Whitcomb 6 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

7. Oscillatory Tidal Effect of GW on a ring of test masses If Interferometer mirrors are the test masses Difference in Path length due to tidal distortion  Interference of laser light at the(Photodiode)

8. Current Status of World-wide GW detection efforts

9. IndIGO - ACIGA meeting9 Laser Interferometer Gravitational-wave Observatory (LIGO)

10. Virgo detector (near Pisa, Italy)

11. LIGO and Virgo TODAY Experimental Milestone: Kilometer scale interferometric GW detectors (LIGO and Virgo) have achieved their predicted design goals. Pre-dawn GW astronomy : Unprecedented sensitivity already allows Upper Limits on GW from a variety of Astrophysical sources. Improve on Spin down of Crab, Vela pulsars..Less than 2% available energy in Crab emitted as GW Experimentally surpass Big Bang nucleosynthesis bound on Stochastic GW..

12. Advanced LIGO

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

14. Mean Expected Annual Coalescence Event Rates Detector Generation NS-NSNS-BHBH-BH Initial LIGO (2002 -2006) 0.020.00060.0009 Advanced LIGO (10X sensitivity) (2014+ - …) 4010.20.0 In a 95% confidence interval, rates uncertain by 3 orders of magnitude NS-NS (0.4 - 400); NS-BH (0.2 - 300) ; BH-BH (2 - 4000) yr^-1 Based on Extrapolations from observed Binary Pulsars, Stellar birth rate estimates, Population Synthesis models. Rates quoted below are mean of the distribution.

15. Need for Long baseline global Network: IndIGO opportunities and benefits

16. 16 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..” Invitation to Present IndIGO case for GWIC Membership on July 10 at GWIC meeting at Cardiff

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

18. LIGO-India: … the opportunity Science Gain from Strategic Geographical Relocation: Source localization error Original Plan 2 +1 LIGO USA+ Virgo LIGO-India plan 1+1 LIGO USA+ Virgo+ LIGO-India LIGO-Aus plan 1+1 LIGO USA+ Virgo+ LIGO-Aus Courtesy: S. Fairhurst

19. Gravitational wave legacy in India Internationally recognized Indian contribution to the global effort for detecting GW on two significant fronts over two decades Seminal contributions to source modeling at RRI [Bala Iyer] and to GW data analysis at IUCAA [Sanjeev Dhurandhar] 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 (LSC) for a decade. At IUCAA, Tarun Souradeep with expertise in CMB data and Planck has worked to create a bridge between CMB and GW data analysis challenges.

20. Indian Gravitational wave strengths Very good students and post-docs produced from this. * Leaders in GW research abroad [Sathyaprakash, Bose, Mohanty] (3) * *New faculty at premier Indian institutions (6) [Gopakumar, Archana Pai, Rajesh Nayak, Anand Sengupta, K.G. Arun, Sanjit Mitra, P. Ajith?] – Gopakumar (Jena  TIFR) and Arun (Virgo  CMI) : 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 characterization schemes, veto techniques for GW transients, bursts, continuous and stochastic sources, radiometric methods, … – P. Ajith (Caltech, LIGO/TAPIR  ? ) …… – Sukanta Bose (Faculty UW, USA  ?) Strong Indian presence in GW Astronomy with Global detector network  broad international collaboration is the norm  relatively easy to get people back.  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 International community reflected in International Advisory committee of IndIGO – Chair Abhay Ashtekar

21. High precision and Large experiment in India TIFR [C.S. Unnikrishnan] : High precision experiments and tests – Test gravitation using most sensitive torsional balances and optical sensors. – Techniques related to precision laser spectroscopy, electronic locking, stabilization. – 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. RRCAT [S.K. Shukla on INDUS] - UHV experience. [Sendhil Raja] - Optical system design, laser based instrumentation, optical metrology, Large aperture optics, diffractive optics, micro-optic system design. [A.S. Raja Rao] (ex RRCAT) - UHV Consultant IPR [S.B. Bhatt on Aditya and Ajai Kumar] - UHV experience. IITM [Anil Prabhakar] and IITK [Pradeep Kumar] (EE depts) – Photonics, Fiber optics and communications – Characterization and testing of optical components and instruments for use in India.. Observatoire de la Cote d'Azur [Rijuparna Chakraborty]..Adaptive Optics.. – Under consideration for postdoc in LIGO or Virgo….

22. Multi-Institutional, Multi-disciplinary Consortium (2009) 1.CMI, Chennai 2.Delhi University 3.IISER Kolkata 4.IISER Trivandrum 5.IIT Madras (EE) 6.IIT Kanpur (EE) 7.IUCAA 8.RRCAT 9.TIFR RRI IPR, Bhatt Jamia Milia Islamia Tezpur Univ

23. The IndIGO Consortium Data Analysis & Theory 1.Sanjeev Dhurandhar IUCAA 2.Bala Iyer RRI 3.Tarun Souradeep IUCAA 4.Anand Sengupta Delhi University 5.Archana Pai IISER, Thiruvananthapuram 6.Sanjit Mitra JPL, IUCAA 7.K G Arun Chennai Math. Inst., Chennai 8.Rajesh Nayak IISER, Kolkata 9.A. Gopakumar TIFR, Mumbai 10.T R Seshadri Delhi University 11.Patrick Dasgupta Delhi University 12.Sanjay Jhingan Jamila Milia Islamia, Delhi 13.L. Sriramkumar, Phys., IIT M 14.Bhim P. Sarma Tezpur Univ. 15.Sanjay Sahay BITS, Goa 16.P Ajith Caltech, USA 17.Sukanta Bose, Wash. U., USA 18.B. S. Sathyaprakash Cardiff University, UK 19. Soumya Mohanty UTB, Brownsville, USA 20.Badri Krishnan Max Planck AEI, Germany Instrumentation & Experiment 1.C. S. Unnikrishnan TIFR, Mumbai 2.G Rajalakshmi TIFR, Mumbai 3.P.K. GuptaRRCAT, Indore 4.Sendhil RajaRRCAT, Indore 5.S.K. Shukla RRCAT, Indore 6.Raja Rao ex RRCAT, Consultant 7.Anil Prabhakar, EE, IIT M 8.Pradeep Kumar, EE, IIT K 9.Ajai Kumar IPR, Bhatt 10.S.K. Bhatt IPR, Bhatt 11.Ranjan Gupta IUCAA, Pune 12.Bhal Chandra Joshi NCRA, Pune 13.Rijuparna Chakraborty, Cote d’Azur, Grasse 14.Rana Adhikari Caltech, USA 15.Suresh Doravari Caltech, USA 16.Biplab Bhawal (ex LIGO) IndIGO Council 1.Bala Iyer ( Chair) RRI, Bangalore 2.Sanjeev Dhurandhar (Science) IUCAA, Pune 3.C. S. Unnikrishnan (Experiment) TIFR, Mumbai 4.Tarun Souradeep (Spokesperson) IUCAA, Pune

24. IndIGO: the goals & roles 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 – Two 4km arm length ultra high vacuum tubes in L configuration – Indian cost ~ Rs 1000Cr The Science & technology benefit of LIGO-India is transformational

25. LIGO-India: Why is it a good idea? … for the World Strategic geographical relocation for GW astronomy – Increased event rates (x4) by coherent analysis – 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 the 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).

26. LIGO-India: Why is it a good idea? … for India – Provides an exciting challenge at an International forefront of experimental science. Can tap and siphon back the extremely good UG students trained in India. (a cause for `brain drain’). – 1 st 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. Symbiotic interplay of Engineering and Science disciplines for a challenging endeavour involving unforgiving technology Jump start direct participation in GW Observations & Astronomy

27. Rewards and Spinoffs Detection of GW is the epitome of breakthrough science!!! 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. Increase number of research groups performing at world class levels and produce skilled researchers. Increase international collaborations in Indian research & establishing Science Leadership in the Asia-Pacific region.

28. … rewards and spinoffs LIGO-India will raise public/citizen profile of science since it will be making ongoing discoveries fascinating the young. GR, BH, EU and Einstein have a special attraction and a pioneering facility in India participating in important discoveries will provide science & technology role models with high visibility and media interest. Einstein@home; Black Hole Hunter… LIGO has a strong outreach tradition and LIGO-India will provide a platform to increase it and synergyesically benefit. Opportune time to a launch 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, path defining, international Experiment in India. A GREAT opportunity but a very sharp deadline of 31 Mar 2012. If we cannot act quickly the possibility will close. Conditions laid out in the Requirement Document 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.

29. Science Payoffs New Astronomy, New Astrophysics, New Cosmology, New Physics ” A New Window ushers a New Era of Exploration in Physics & Astronomy” – 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 cosmic events.. Supernovae, Gamma-ray bursts, LMXB’s, Magnetars – New cosmology..SMBHB’s as standard sirens..EOS of Dark Energy – Phase transition related to fundamental unification of forces – Multi-messenger astronomy – The Unexpected !!!!!

30. Unique 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 : New technology for other fields Vibration Isolation and suspension.. Applications for mineral prospecting Squeezing and challenging “quantum limits” in measurements. Largest Ultra-high vacuum system 10^-9 torr (1picomHg) in the region. Such a UHV system will provide industry a challenge and experience. Computation Challenges: Cloud computing, Grid computing, new hardware and software tools for computational innovation.

31. END Thank you !!! Thank you !!! Part I Part I Over to Tarun… Over to Tarun…

32. vit GWIC Roadmap Document Gravitational wave Astronomy : Synergy with other major Astronomy projects SKA : Pulsars timing and GW background, GW from Pulsars,… ( RADIO: Square Kilometer array) CMB : GW from inflation, cosmic phase transitions, dark energy …. (Cosmic Microwave Background : WMAP, Planck, CMBPOl, QUaD,…) X-ray satellite (AstroSat) : Spacetime near Black Holes, NS, …. Gamma ray observatory: GRB triggers from GW (FermiLAT, GLAST,….) Thirty Meter Telescope: Resolving multiple AGNs, optical follow-up, … INO: cross correlate neutrino signals from SN event LSST: Astro-transients with GW triggers, Cosmic distribution of dark matter, Dark energy

33. 23 July 2011 Dear Bala: to present the GWIC membership application for IndIGO. you have made a strong case for membership…… 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…… Invitation to Present IndIGO case for GWIC Membership on July 10 at GWIC meeting at Cardiff

34. IndIGO 3m Prototype Detector Funded by TIFR Mumbai on compus (2010) PI: C. S. Unnikrishnan (Cost ~ INR 2.5 crore)

35. LIGO-India: … the opportunity Polarization info Homogeneity of Sky coverage Courtesy: S.Kilmenko & G. Vedovato Strategic Geographical relocation: science gain

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

37. 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 (ACIGA &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 (ACIGA&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), [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)]

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

39. NetworkHHLVHILVAHLV Mean horizon distance 1.741.571.69 Detection Volume 8.988.778.93 Volume Filling factor 41.00%54.00%44.00% Triple Detection Rate(80%) 4.865.956.06 Triple Detection Rate(95%) 7.818.138.28 Sky Coverage: 81% 47.30%79.00%53.50% Directional Precision 0.662.023.01 Strategic Geographical relocation: science gain

40. 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. Space Time as a fabric

41. Earth follows a “straight path” in the curved space-time caused by sun’s mass !!!

42. What happens when matter is in motion?

43. 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

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

45. Concluding remarks A century after Einstein’s prediction, we are on the threshold of a new era of GW astronomy following GW detection. Involved four decades of very innovative and Herculean struggle at the edge of science & technology First generation detectors like Initial LIGO and Virgo have achieved design sensitivity  Experimental field is mature Broken new ground in optical sensitivity, pushed technology and proved technique. Second generation detectors are starting installation and expected to expand the “Science reach” by factor of 1000 Cooperative science model: A worldwide network is starting to come on line and the ground work has been laid for operation as a integrated system. Low project risk : A compelling Science case with shared science risk, a proven design for India’s share of task (other part : opportunity w/o responsibility) National mega-science initiative: Need strong multi-institutional support to bring together capable scientists & technologist in India An unique once-in-a-generation opportunity for India. India could play a key role in Intl. Science by hosting LIGO-India.

46. … Concluding remarks A GREAT opportunity but a very sharp deadline of 31 Mar 2012. If we cannot act quickly the possibility will close. Conditions laid out in the Request 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.

47. 47 Initial LIGO Sensitivity Goal Strain sensitivity <3x10 -23 1/Hz 1/2 at 200 Hz l Sensor Noise »Photon Shot Noise »Residual Gas l Displacement Noise »Seismic motion »Thermal Noise »Radiation Pressure

48. Advanced LIGO Take advantage of new technologies and on-going R&D >> Active anti-seismic system operating to lower frequencies: (Stanford, LIGO) >> 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 Design: 1999 – 2010 : 10 years of high end R & D internationally. Construction: Start 2008; Installation 2011; Completion 2015

49. A Century of Waiting Almost 100 years since Einstein predicted GW but no direct experimental confirmation (a la Hertz for Maxwell EM theory) 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 any Detector GW Hertz experiment ruled out. Only astrophysical systems involving huge masses and accelerating very strongly are potential detectable sources of GW signals.

50. Astrophysical systems are sources of copious GW emission: GW emission efficiency (10% of mass for BH mergers) >> EM radiation via Nuclear fusion (0.05% of mass) Energy/mass 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 GW  Astronomy link

51. 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

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

53. Principle behind Detection of GW

54. Courtesy: Stan Whitcomb end test mass beam splitter signal LIGO Optical Configuration Laser Michelson Interferometer Michelson Interferometer input test mass Light is “recycled” about 50 times Power Recycled with Fabry-Perot Arm Cavities Light bounces back and forth along arms about 100 times Detecting GW with Laser Interferometer Difference in distance of Paths  Interference of laser light at the detector (Photodiode)

55. Dear Prof. Kasturirangan, 1 June 2011 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. 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. 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. operational early in the lifetime of the advanced versions of gravitational wave observatories India would be unique among nations leading the scientific exploration of this new window on the universea fraction of the total cost of independently establishing a fully-equipped and advanced observatory. 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 from LIGO

56. Pulsar companion Binary Pulsars..NS-NS Binary High quality observational data that GW exist….