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LIGO-India

IndIGO Consortium ( Ind ian I nitiative in G ravitational-wave O bservations). LIGO-India. Tarun Souradeep, IUCAA (Spokesperson, IndIGO). LIGO Detector at Hanford USA. An Indo-US joint mega-project concept proposal. www.gw-indigo.org.

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LIGO-India

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  1. IndIGO Consortium (Indian Initiative in Gravitational-wave Observations) LIGO-India Tarun Souradeep, IUCAA (Spokesperson, IndIGO) LIGO Detector at Hanford USA An Indo-US joint mega-project concept proposal www.gw-indigo.org

  2. Gravitational waves & experimental effortsto detect them!!!

  3. Beauty & Precision Einstein’s General theory of relativity is considered the most beautiful, as well as, successful theory of modern physics. It has matched all weak field experimental tests of Gravitation in the solar system remarkably well… TouTouches everyday Life too…GPS

  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. • GW are a major qualitatively unique prediction beyond Newton’s gravitation • Any theory of Gravitation consistent with Special Relativity will lead to GW…However, the properties of GW in different theories of gravity could be different …

  5. Astrophysical Sources for Terrestrial GW Detectors • Compact binary Coalescence: “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

  6. Gravitational wave Astronomy : vit GWIC Roadmap Document

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

  8. Mean Expected Annual Coalescence Event Rates 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.

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

  10. LIGO-India:a good idea for GW community ! • Geographical relocation Strategic for GW astronomy • Increased event rates (x2-4) by coherent analysis • Improved duty cycle • Improved Detection confidence • Improved Sky Coverage • Improved Source Location required for multi-messenger astronomy • Improved Determination of the two GW polarizations • Potentially large Indian science user community in the future • Indian demographics: youth dominated – need challenges • Improved UG education system will produce a larger number of students with aspirations looking for frontline research opportunity at home. • Substantial data analysis trained faculty exists in India and Large Data Analysis Center Facilities are being planned under the next five year plan for consolidated IndIGO participation in LSC for Advanced LIGO

  11. LIGO-India:Attractive Indian megaproject • On Indian Soil with International Cooperation (no competition) • Shared science risks and credits with the International community. • AdvLIGO setup & initial setup risks primarily rests with USA. • AdvLIGO-USA precedes LIGO-India by > 2 years. • Vacuum 10 yr of operation in initial LIGO  2/3 vacuum enclosure + 1/3 detector assembly split (US ‘costing’ : manpower and h/ware costs) • Indian expters can contribute to AdvLIGO-USA : opportunity without primary responsibility • US hardware contribution funded & ready • AdvLIGO largest NSF project funded in USA • LIGO-India needs NSF approval, but not additional funds from USA • Expenditure almost completely in Indian labs & Industry • Very significant Industrial capability upgrade in India. • Well defined training plan  Large number of highly trained HRD • Host a major data analysis facility for the entire LIGO network

  12. LIGO-India: … the opportunity Science Gain from Strategic Geographical Relocation Source localization error Courtesy: S. Fairhurst 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

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

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

  15. LIGO-India: … the challenges • Indian contribution in human resources: • Trainable Scientific & engineering manpower for detector assembly, installation and commissioning. • Trained S & T manpower for LIGO-India sustained operations for next 10 years. • Major enhancement of Data Analysis team. Seek Consolidated IndIGO participation in LIGO Science Collab. (Sept 2011) • Expand theory and create numerical relativity simulation. Expect a significant number of hirings in premier institutions

  16. LIGO-India: … the challenges • Indian contribution in Engineering. & infrastructure: • Ultra-high Vacuum enclosure on large scale • Site (L-configuration: Each 100-200 m x 4.5km: < 300 acres) • HPC -Data centre

  17. LIGO-India: … the challenges Indian Site • Requirements: • Low seismicity • Low human generated noise • Air connectivity • Proximity to Academic institutions, labs, industry preferred, … • Identify potential sites not too far from existing facilities • Need to carry out seismic survey to get ground noise spectral density at 0.1-10 Hz range • Few interesting possibilities are under investigation

  18. Large scale ultra-high Vacuum • Fabricated and installed by Indian Industry under close monitoring by science & technology team • Oversee the procurement & fabrication of the vacuum system components and its installation by a national multi-institutional team. • DAE commitment to LIGO-India  Intense participation of RRCAT & IPR possible. • All vacuum components such as flanges, gate-valves, pumps, residual gas analyzers and leak detectors will be bought. • Companies L&T, Fullinger, HindHiVac, Godrej, … with close support from RRCAT, IPR and LIGO Lab. • Preliminary detailed discussions with Industry in Feb 2011 :Companies like HHV, Fullinger, Godrej 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 component is INR 400 cr. (~80 M USD)

  19. Detector Assembly & Commissioning For installation and commissioning phase: • Identify 10-15 core experienced Enggs. & scientists who spend a year, or more, at Advanced LIGO-USA during its install. & comm. • LIGO proposal document • Already 1 IndIGO post-doc at LIGO Caltech, 2 others under consideration in LIGO and EGO,.. • Creste positions back in India for them (Once project manpower sanctioned, LIGO-India project hiring at institutions like RRCAT, TIFR, IUCAA,….) • 6-10 full time engineers and scientists in India. Present experimental expertise within IndIGO Laser ITF: TIFR, RRCAT, IITM, IIT K. UH Vacuum: RRCAT, IPR, (TIFR, IUCNS, new IUCs? ) Each group can scale to 10 Post-doc/PhD students. Over 2-3 years. Train on 3-m prototype .

  20. Thank you !!! Concluding Remarks.. • Over two decades India has been involved in quality GW research and been a part of the International GW community • Since 2009 Indian aspirations involve participation in a major GW experiment eventually leading to a GW detector in India • With immense help & encouragement from the International GW community, IndIGO has made significant progress to integrate India into the GWIC road map towards the setting up of a Global GW detector network • IndIGO is actively pursuing concrete, ambitious, well supported plans to revamp the scale and scope of Indian participation in GW research and GW Astronomy in the coming decades. **All interested researchers are welcome to join our efforts**

  21. LIGO-India: unique once-in-a-generation opportunity LIGO labs LIGO-India ?

  22. Advanced LIGO Laser • Unique globally. Well beyond current Indian capability. Would require years of focused R &D effort. Both power and frequency stability ratings. • AdvLIGO laser has spurred RRCAT to envisage planning development of similar laser capability in the next 5 year plans. IIT M group also interested. • Multiple applications of narrow line width laser : Freq time stand, precision metrology, Quantum key distribution, high sensitivity seismic sensors (geo sc.), coherence LIDAR (atm sc.), …. • Designed and contributed by Albert Einstein Institute, Germany • Much higher power (to beat down photon shot noise) • 10W  180W (narrow sub kHz line width) • Better stability • 10ximprovement in intensity (nano ppm) and frequency stability (mHz) Courtesy: Stan Whitcomb

  23. Advanced LIGO Mirrors • Surface specs (/1000) : 100 x best optical telescope • Surface specs currently available in India for much smaller sizes /20 • Indian industry may now be challenged to achieve on small scale, eg., for TIFR 3m prototype • Technology for such mirror useful for high optical metrology and other specialized applications • Feb 2011 Status • All substrates delivered • Polishing underway • Reflective Coating process starting up • Larger size • 11 kg  40 kg, 2534 cm • Smaller figure error • 0.7 nm  0.35 nm • Lower absorption • 2 ppm 0.5 ppm • Lower coating thermal noise Courtesy: Stan Whitcomb

  24. Advanced LIGO Seismic Isolation • Unique design • New benchmark for isolation experiments in India : gravitation, Space sensor appls.… • Application in various industrial and lab test centers • 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

  25. Advanced LIGO Suspensions four stages 40 kg silica test mass 25 • 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 • resonance subHz • suppression 1/f^4 per stage (6 stages) Courtesy: Stan Whitcomb

  26. LIGO-India: unique once-in-a-generation opportunity • “Quantum measurements” • to improve further via squeezed light: • Potential technology spin-offs will impact quantum computing and quantum key distribution (QKD) for secure communications. (IITM approached by ITI for QKD development.) • New ground for optics and communication technology in India • High Potential to draw the best Indian UG students, typically interested in theoretical physics, into experimental science !!!

  27. LIGO-India: … the challenges • Indian contribution in human resources: • Trained Scientific & engineering manpower for detector assembly, installation and commissioning (2.) • Trained SE manpower for LIGO-India sustained operations for next 10 years (3.) • Major enhancement of Data Analysis team. Seek Consolidated IndIGO participation in LIGO Science Collab. (Sept 2011) • Expand theory and create numerical relativity simulation. Expect hiring in premier institutions

  28. Participation in LSC during Advanced LIGOProposed Data Analysis activities of the IndIGO Consortium • Principal Leads: K.G. Arun, R.Nayak, A. Pai, A. Sengupta, S. Mitra • Participants: S. Dhurandhar, T. Souradeep, B. R. Iyer, C.K. Mishra, • M.K. Harris,…. • Institutions: CMI, IUCAA, IISER (Kolkata), IISER (Tvm), Univ Delhi • Projects • Multi-detector Coherent veto • Tests of GR and alternative theories of gravity • Stochastic Gravitational wave background analysis • IndIGO Data Center

  29. IndIGO Data Centre @ IUCAA Anand Sengupta, DU, IndIGO • Primary Science: Online Coherent search for GW signal from binary mergers using data from global detector network Coherent  2-4 x event rate (40  80-160 /yr for NS-NS) • Role of IndIGO data centre • Large Tier-2 data/compute centre for archival of GW data and analysis • Bring together data-analysts within the Indian gravity wave community. • Puts IndIGO on the global map for international collaboration with LIGO Scientific Collaboration. Facility for LSC as part of IndIGO participation. • Large University sector participation via IUCAA • 200 Tflops peak capability (by 2014) • Storage: 4x100TB per year per interferometer. • Network: gigabit+ backbone, National Knowledge Network • Gigabit dedicated link to LIGO lab Caltech • 20 Tf 200 Tb funded by IUCAA : ready Mid 2012

  30. Indo-US centre for Gravitational Physics and Astronomy @ IUCAA APPROVED (Dec 2010). Funds received Jul 6, 2011 • Centre of Indo-US Science and Technology Forum (IUSSTF) • Exchange program to fund mutual visits and facilitate • interactions leading to collaborations • Nodal centres: IUCAA , Pune, India & Caltech, Pasadena, USA. • Institutions: • Indian: IUCAA, TIFR, IISER, DU, CMI - PI: Tarun Souradeep • USA: Caltech, WSU - PI: Rana Adhikari

  31. Strategic Geographical relocation: science gain Courtesy: Bernard Schutz

  32. High precision experimental expertise in India • TIFR : High precision experiments and tests of weak forces [C.S. Unnikrishnan] • Test gravitation using most sensitive torsional balances and optical sensors. • Techniques related to precision laser spectroscopy, electronic locking, stabilization. • G.Rajalakshmi (IIA  TIFR, 3m prototype); • Suresh Doravari (IIA  LIGO, Caltech 40m/Adv LIGO) • RRCAT (RR Center for Advanced Tech.) • [S.K. Shukla on INDUS, A.S. Raja Rao (ex RRCAT)] --UHV • [Sendhil Raja, P.K. Gupta] - Optical system design, laser based instrumentation, optical metrology, Large aperture optics, diffractive optics, micro-optic system design. • [Rijuparna Chakraborty, France  LIGO/EGO pdf?]Adaptive Optics…. • IPR (Institute for Plasma Research) • [S.B. Bhatt on Aditya and Ajai Kumar] - UHV , Lasers, Control systems,.. • 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..

  33. Large experiment expertise in India • Groups at BARC (Bhabha Atomic Res. Center) and RRCAT : involved in LHC hardware contribution • provided 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. • Teams at Electronics & Instrumentation Groups at BARC (may be interested in large instrumentation projects in XII plan) • IPR (Inst. for Plasma res.): Involved in ITER (6xLIGO-Ind cost) Support role in large volume UHV system, Control systems,…. • Groups at ISRO (Ind. Space Res. Org.) ,……. Control systems, Clean rooms, Large scale fabrication, ...... • Over the last two years contacts made with the above groups  opportunities in a GW experiment and explore their possible participation in LIGO-India/Aus.

  34. Multi-Institutional, Multi-disciplinary Consortium (Aug. 2009) Nodal Institutions • CMI, Chennai • Delhi University • IISER Kolkata • IISER Trivandrum • IIT Madras (EE) • IIT Kanpur (EE) • IUCAA, Pune • RRCAT, Indore • TIFR, Mumbai • IPR, Bhatt • Others • RRI • JamiaMiliaIslamia • TezpurUniv

  35. 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 . Sanjay Sahay BITS, Goa 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 Bhal Chandra Joshi NCRA, Pune Rijuparna Chakraborty, Cote d’Azur, Grasse Rana Adhikari Caltech, USA Suresh Doravari Caltech, USA Biplab Bhawal (ex LIGO) Sunil (IPR/UWA)

  36. IndIGO: Goals & current activities • Provide a common umbrella to initiate and expand GW related experimental activity and train new technically skilled manpower • Seeking pan-Indian consolidated IndIGO membership in LIGO Scientific Collaboration (LSC) for participation in Advanced LIGO. • Create a Tier-2 data centre in IUCAA for LIGO Scientific Collaboration Deliverables and as a LSC Resource • Starting collaborative work under the IUSSTF Indo-US IUCAA-Caltech joint Centre at IUCAA • Indo-Jap project “Coherent multi-detector gravitational wave search using LCGT and advanced interferometers” • Explore the Roadmap for EGO-IndIGO collaboration on GW and a possible MOU (Meeting on Nov 1-2 ,2011 at IUCAA) • Explore Indian participation in LISA and space based GW detectors in the future ( ASTROD 5 meeting on July 14 – 16, 2012 at RRI)

  37. IndIGO Consortium – a brief history • Dec. 2007 : ICGC2007 @IUCAA: RanaAdhikari’s visit & discussions • 2009: • Australia-India S&T collaboration (Iyer & Blair) Establishing Australia-India collaboration in GW Astronomy • IndIGO Consortium: Reunion meeting IUCAA (Aug 9, 2009) • GW Astronomy Roadmap for India; • 2009-2011: • Meetings at Kochi, Pune, Shanghai, Perth, Delhi to Define, Reorient and Respond to the Global (GWIC) strategies for setting up the International GW Network. • Bring together scattered Indian Experimental Expertise; Individuals & Institutions • March 2011: IndIGO-I Proposal: Participation in LIGO-Australia • May 2011+: LIGO-India..

  38. IndIGO: the Aspiration • Create major Indian presence in GW astronomy • MOU with ACIGA to collaborate on GW Astronomy • Partner in LIGO-Australia • Indian partnership at 15% of Australian cost with full data rights A significant recent development … • LIGO-India • Letter from LIGO Lab. with a concept proposal for LIGO-India • LIGO-India is under preliminary consideration for National Mega Projects under the forthcoming Five year plan in India .

  39. RRCAT (Next Plan period): Advanced Interferometry(Narrow line width Frequency Stabilised laser development) The laser will be an injection seeded Nd;YAG or Yb:Silica fiber laser locked to a stabilized reference cavity. The target would be to demonstrate a laser with 1W output and sub-kHz line width and few Hz stability. Scaling up of the power to 10W will be done as the next step.

  40. RRCAT: Advanced Interferometry(Ultraflat Components development) Development of Ultraflat Optical components such as mirrors for GWD will require augmenting the existing facility with an ion beam figuring system for final correction of the polished optics to /500 or better.

  41. Photonics @ IIT-Madras (& IIT- Kanpur) 11 faculty members (8 in EE, 3 in Physics) 10 M. Tech scholars in EE (Photonics) 20+ research scholars (M.S. and Ph.D.) Research specializations • Optical communications • Fiber lasers • Diffractive optical elements • Silicon photonics, plasmonics • Nonlinear and quantum optics • Metrology and instrumentation Strong industry partnerships

  42. IndIGO 3m Prototype Detector Funded by TIFR Mumbai on campus (2010)PI: C. S.Unnikrishnan ( INR 3.5cr ~.7 M$ ) • Goals of the TIFR 3-m prototype interferometer (to be operational in 2014): • Research and Training platform with all the features of the advanced LIGO-like detectors, scaled down to displacement sensitivity around 10-18 m, above 200 Hz. • The Indian research platform for features like signal recycling, DC read-out, and most importantly the use of squeezed light and noise reduction (last phase). • Instrument for studies on short range gravity and QED force, especially a measurement of the Casimir force in the range 10 -100 microns where no previous measurements exist (Rajalakshmi and Unnikrishnan, Class, Quant. Grav. 27, 215007 (2010).

  43. 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

  44. Gravitational wave Astronomy : vit • 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 GWIC Roadmap Document

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