1. 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: 1R Jun 17, 2011 : TS www.gw-indigo.org

2. 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

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

4. Beauty & Precision

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. 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 GW  Astronomy link

9. Pulsar companion GW from Binary Neutron stars

10. leads to loss of orbital energy period speeds up 14 sec from 1975-94 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 Gravity waves Nobel prize in 1993 !!!

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

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

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

16. Courtesy: Stan Whitcomb16 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

17. 17 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

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. IndIGO - ACIGA meeting19 Laser Interferometer Gravitational-wave Observatory (LIGO)

20. Courtesy;: Stan Whitcomb 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

21. 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.

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: New ground for optical technologists in India High Potential to draw the best Indian UG students typically interested in theoretical physics into experimental science !!!

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 LASER AEI, Hannover Germany Seismic isolation Suspension GEO, UK Reflects International cooperation Basic nature of GW Astronomy

26. Courtesy: Stan Whitcomb26 Advanced LIGO Laser Designed and contributed by Albert Einstein Institute< Germany Higher power – 10W -> 180W Better stability – 10x improvement in intensity and frequency stability

27. Courtesy: Stan Whitcomb27 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

28. 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

29. Courtesy: Stan Whitcomb29 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 ~10 5 -> ~10 8 Suppression at 10 Hz : ? at 1 Hz : ? 29 40 kg silica test mass four stages

30. 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-NSNS-BHBH-BH Initial LIGO (2002 -2006) 0.020.00060.0009 Enhanced LIGO (2X Sensitivity) (2009-2010) 0.10.040.07 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.

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

34. 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. vit GWIC Roadmap Document Gravitational wave Astronomy : 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

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-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

41. 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.P Ajith Caltech, USA 16.Sukanta Bose, Wash. U., USA 17.B. S. Sathyaprakash Cardiff University, UK 18. Soumya Mohanty UTB, Brownsville, USA 19.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.Rijuparna Chakraborty, Cote d’Azur, Grasse 13.Rana Adhikari Caltech, USA 14.Suresh Doravari Caltech, USA 15.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

42. 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……

43. Committees: National Steering Committee: Kailash Rustagi (IIT, Mumbai) [Chair] Bala Iyer (RRI) [Coordinator] Sanjeev Dhurandhar (IUCAA) [Co-Coordinator] D.D. Bhawalkar (Quantalase, Indore)[Advisor] P.K. Kaw (IPR) Ajit Kembhavi (IUCAA) P.D. Gupta (RRCAT) J.V. Narlikar (IUCAA) G. Srinivasan International Advisory Committee Abhay Ashtekar (Penn SU)[ Chair] Rana Adhikari (LIGO, Caltech, USA) David Blair (AIGO, UWA, Australia) Adalberto Giazotto (Virgo, Italy) P.D. Gupta (Director, RRCAT, India) James Hough (GEO ; Glasgow, UK)[GWIC Chair] Kazuaki Kuroda (LCGT, Japan) Harald Lueck (GEO, Germany) Nary Man (Virgo, France) Jay Marx (LIGO, Director, USA) David McClelland (AIGO, ANU, Australia) Jesper Munch (Chair, ACIGA, Australia) B.S. Sathyaprakash (GEO, Cardiff Univ, UK) Bernard F. Schutz (GEO, Director AEI, Germany) Jean-Yves Vinet (Virgo, France) Stan Whitcomb (LIGO, Caltech, USA) IndIGO Advisory Structure Program Management Committee: C S Unnikrishnan (TIFR, Mumbai), [Chair] Bala R Iyer (RRI, Bangalore), [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. 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 3m Prototype Detector Funded by TIFR Mumbai on compus (2010) PI: C. S. Unnikrishnan (Cost ~ INR 2.5 crore)

46.  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 IndIGO Data Centre@IUCAA

47. Indo-US centre for Gravitational Physics and Astronomy Centre of Indo-US Science and Technology Forum (IUSSTF) Exchange program to fund mutual visits and facilitate interaction. Nodal centres: IUCAA, India & Caltech, US. Institutions: Indian: IUCAA, TIFR, IISER, DU, CMI - PI: Tarun Souradeep US: Caltech, WSU - PI: Rana Adhikari APPROVED for funding (Dec 2010)

48. 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

49. 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’). – 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. – 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.

50. 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.

51. LIGO-India: Salient points of this megaproject On Indian Soil will draw and retain science & tech. manpower International Cooperation, not competition LIGO-India success critical to the success of the global GW science effort. Complete Intl support Shared science risk with International community  Shared historical, major science discovery credit !!! AdvLIGO setup & initial challenge/risks primarily rests with USA. – AdvLIGO-USA precedes LIGO-India by > 2 years. – India sign up for technically demonstrated/established part (>10 yr of operation in initial LIGO )  2/3 vacuum enclosure + 1/3 detector assembly split (US ‘costing’ : manpower and h/ware costs) – However, allows Indian scientist to collaborate on highly interesting science & technical challenges of Advanced LIGO-USA ( *** opportunity without primary responsibility ***) Expenditure almost completely in Indian labs & Industry huge potential for landmark technical upgrade in all related Indian Industry Well defined training plan core Indian technical team thru Indian postdoc in related exptal areas participation in advLIGO-USA installation and commissioning phase, cascade to training at Indian expt. centers Major data analysis centre for the entire LIGO network with huge potential for widespread University sector engagement. US hardware contribution funded & ready advLIGO largest NSF project, LIGO-India needs NSF approval but not additional funds

52. LIGO-India: … the opportunity Strategic Geographical relocation: science gain 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

53. LIGO-India: … the opportunity Polarization info Homogeneity of Sky coverage Courtesy: B. Schutz Strategic Geographical relocation: science gain

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

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

56. 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

57. LIGO-India: unique once-in-a-generation opportunity LIGO labs  LIGO-India 180 W pre-stabilized Nd:YAG laser 10 interferometer core optics (test masses, folding mirrors, beam splitter, recycling mirrors) 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. 5 "BSC chamber" seismic isolation systems (two stage, six degree of freedom, active isolation stages capable of ~200 kg payloads) 6 "HAM Chamber" seismic isolation systems (one stage, six degree of freedom, active isolation stages capable of ~200 kg payloads) 11 Hydraulic External Pre-Isolation systems 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

58. LIGO-India vs. Indian-IGO ? Primary advantage: LIGO-India Provides cutting edge instrumentation & technology to jump start GW detection and astronomy. Would require at least a decade of focused & sustained technology developments in Indian laboratories and industry 180 W Nd-Yag: 5 years; Rs. 10-12 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.. 3-4 years of development.. Not trivial to implement. – Benefit other physics experiments working at the quantum limit of noise.

59. LIGO-India: Expected Indian Contribution Indian contribution in infrastructure:  Site (L-configuration: Each 50-100 m x 4.2 km)  Vacuum system  Related Controls  Data centre Indian contribution in human resources:  Trained manpower for installation and commissioning  Trained manpower for LIGO-India operations for 10 years  Simulation and Data Analysis teams

60. The 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 !!!!!

61. 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 : New technology for other fields Vibration Isolation and suspension.. Applications for mineral prospecting Squeezing and challenging “quantum limits” in measurements. Ultra-high vacuum system 10^-9 tor (1picomHg). Beyond best in the region Computation Challenges: Cloud computing, Grid computing, new hardware and software tools for computational innovation.

62. The 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. The largest UHV system will provide industry a challenge and experience.

63. … 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. LIGO has a strong outreach tradition and LIGO-India will provide a platform to increase it and synergetically 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 & establishing Science Leadership in the Asia-Pacific region.

64. 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

65. 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)

66. Logistics and Preliminary 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, LIGO- India project hiring at RRCAT, TIFR, other insitututions/Labs.

67. 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 10000m 3 (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

68. 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 (vacuum 400 cr) Large scale ultra-high Vacuum enclosure

69. Logistics and Preliminary Plans 42 persons (10 PhD/postdocs, 22 scientists/engineers and 10 technicians) 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) – 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 – 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.

70. … Logistics and Work Plan Teams at Electronics & Instrumentation Groups at BARC may be interested in 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 Construction – 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.

71. LIGO-India: … the challenges Manpower generation for sustenance of the LIGO-India observatory : Preliminary Plans & 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 IndIGO Summer internships in International labs underway o High UG applications 30/40 each year from IIT, IISER, NISERS,.. o 2 summers, 10 students, 1 starting PhD at LIGO-MIT o Plan to extend to participating National labs to generate more experimenters IndIGO schools are planned annually to expose students to emerging opportunity in GW science o 1 st IndIGO school in Dec 2010 in Delhi Univ. (thru IUCAA) Post graduate school specialization courses, or more 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.”

72. LIGO-India: … the challenges Indian Site 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

73. 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.

74. … 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.

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