LIGO-India Detecting Einstein’s Elusive Waves Opening a New Window to the Universe
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Transcript of LIGO-India Detecting Einstein’s Elusive Waves Opening a New Window to the Universe
LIGO-IndiaDetecting Einstein’s Elusive Waves
Opening a New Window to the Universe
An Indo-US joint mega-project concept proposal
IndIGO Consortium(Indian Initiative in Gravitational-wave Observations)
Version: 4 Jun 14, 2011 - BRIwww.gw-indigo.org
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
Space Time as a fabric
Earth follows a straight line in the curved space-time caused by sun’s mass !!!
Einstein’s General theory of relativity is the most beautiful, as well as,
successful theory of modern physics.
It has matched all experimental tests of Gravitation remarkably well.
Era of precision tests : GP-B,….
Beauty & Precision
What happens when matter is in motion?
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 !!!
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.
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 eventsBursts (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
Pulsar companion
GW from Binary Neutron stars
• 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 TaylorResults for PSR1913+16
Indirect evidence for Gravity waves
Nobel prizein 1993 !!!
Principle behind Detection of GW
Effect of GW on a ring of test masses
Interferometer mirrors as test masses
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
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
Challenge of Direct Detection
2 L hL
20 2410 10h
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!
Courtesy: Stan Whitcomb 16
end test mass
beam splittersignal
LIGO Optical Configuration
Laser
MichelsonInterferometer
input test massLight is “recycled” about 50 times
Power Recycled
with Fabry-Perot Arm Cavities
Light bounces back and forth along arms about 100 times
17
Initial LIGO Sensitivity Goal
• Strain sensitivity <3x10-23 1/Hz1/2
at 200 Hz
Sensor Noise» Photon Shot Noise» Residual Gas
Displacement Noise» Seismic motion» Thermal Noise» Radiation Pressure
LIGO and Virgo TODAYMilestone: Decades-old plans to build and operate large interferometric GW detectors now realized at several locations worldwideExperimental 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..
IndIGO - ACIGA meeting 19
Laser Interferometer Gravitational-wave Observatory (LIGO)
20Courtesy;: Stan Whitcomb
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
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 andIUCAA in its Data Analysis Aspects.
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
“Quantum measurements” to improve further via squeezed light:
A big draw for the large Indian theoretical physics community & students !!!
(& of course, optics technology)
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
Schematic Optical Design of Advanced LIGO detectors
LASERAEI, Hannover
Germany
Seismic isolation Suspension
GEO, UK
Reflects International cooperationBasic nature of GW Astronomy
Courtesy: Stan Whitcomb 26
Advanced LIGO Laser• Designed and contributed by Albert Einstein Institute<
Germany• Higher power
– 10W -> 180W• Better stability
– 10x improvement in intensity and frequency stability
Courtesy: Stan Whitcomb 27
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
28Courtesy: Stan Whitcomb
Advanced LIGO Seismic Isolation• Two-stage six-degree-of-freedom active isolation
– Low noise sensors, Low noise actuators– Digital control system to blend outputs of multiple sensors,
tailor loop for maximum performance– Low frequency cut-off: 40 Hz -> 10 Hz
Courtesy: Stan Whitcomb 29
Advanced LIGO Suspensions
• UK designed and contributed test mass suspensions
• Silicate bonds create quasi-monolithic pendulums using ultra-low loss fused silica fibres to suspend interferometer optics
– Pendulum Q ~105 -> ~108
Suppression at 10 Hz : ?
at 1 Hz : ?
29
40 kg silica test mass
four stages
Era of Advanced LIGO detectors: 2015
10x sensitivityÞ10x reach
Þ 1000 volume>> 1000 event rate
(reach beyondnearest super-
clusters)A Day of Advanced
LIGO Observation >> A year of Initial LIGO
Expected Annual Coalescence Event RatesDetector Generation
NS-NS NS-BH BH-BH
Initial LIGO(2002 -2006) 0.02 0.0006 0.0009
Enhanced LIGO(2X Sensitivity)(2009-2010)
0.1 0.04 0.07
Advanced LIGO(10X sensitivity)(2014 - …) 40 10. 20.0
In a 95% confidence interval, rates uncertain by 3 orders of magnitudeNS-NS (0.4 - 400); NS-BH (0.2 - 300) ; BH-BH (2 - 4000) yr^-1
Based on Extrapolations from observed Binary Pulsars, Stellar birth rateestimates, Population Synthesis models. Rates quoted below are mean of the distribution.
Scientific PayoffsAdvanced 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
GW Astronomy with Intl. Network of GW Observatories
LIGO-LLO: 4km
LIGO-LHO: 2km+ 4kmGEO: 0.6km VIRGO: 3km
LCGT 4kmTAMA/CLIO
LIGO-Australia?
1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info.
LIGO-India ?
34
From the GWIC Strategic Roadmap for GW Science with thirty year horizon (2007)
• … the first priority for ground-based gravitational wave detector development is to expand the network, adding further detectors with appropriately chosen intercontinental baselines and orientations to maximize the ability to extract source information. ….Possibilities for a detector in India (IndIGO) are being studied..
Indo-Aus.Meeting, Delhi, Feb 2011
vit
Courtesy: B. Schutz, GWIC Roadmap Document 2010
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• •
The Gravitational wave legacyTwo 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.
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
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….
Multi-Institutional,Multi-disciplinary Consortium(2009)
1. CMI, Chennai2. Delhi University3. IISER Kolkata4. IISER Trivandrum5. IIT Madras (EE)6. IIT Kanpur (EE)7. IUCAA8. RRCAT9. TIFR
• RRI• IPR, Bhatt• Jamia Milia Islamia• Tezpur Univ
The IndIGO Consortium
Data Analysis & Theory
1. Sanjeev Dhurandhar IUCAA2. Bala Iyer RRI3. Tarun Souradeep IUCAA4. Anand Sengupta Delhi University 5. Archana Pai IISER, Thiruvananthapuram6. Sanjit Mitra JPL , IUCAA7. K G Arun Chennai Math. Inst., Chennai8. Rajesh Nayak IISER, Kolkata9. A. Gopakumar TIFR, Mumbai 10. T R Seshadri Delhi University 11. Patrick Dasgupta Delhi University12. Sanjay Jhingan Jamila Milia Islamia, Delhi13. L. Sriramkumar, Phys., IIT M14. Bhim P. Sarma Tezpur Univ . 15. P Ajith Caltech , USA16. Sukanta Bose, Wash. U., USA17. B. S. Sathyaprakash Cardiff University, UK18. Soumya Mohanty UTB, Brownsville , USA19. Badri Krishnan Max Planck AEI, Germany
Instrumentation & Experiment
1. C. S. Unnikrishnan TIFR, Mumbai2. G Rajalakshmi TIFR, Mumbai3. P.K. Gupta RRCAT, Indore 4. Sendhil Raja RRCAT, Indore5. S.K. Shukla RRCAT, Indore6. Raja Rao ex RRCAT, Consultant 7. Anil Prabhakar, EE, IIT M8. Pradeep Kumar, EE, IIT K9. Ajai Kumar IPR, Bhatt10. S.K. Bhatt IPR, Bhatt 11. Ranjan Gupta IUCAA, Pune12. Rijuparna Chakraborty, Cote d’Azur, Grasse13. Rana Adhikari Caltech, USA 14. Suresh Doravari Caltech, USA 15. Biplab Bhawal (ex LIGO)
IndIGO Council1. Bala Iyer ( Chair) RRI,
Bangalore 2. Sanjeev Dhurandhar (Science) IUCAA, Pune 3. C. S. Unnikrishnan (Experiment) TIFR, Mumbai4. Tarun Souradeep (Spokesperson) IUCAA, Pune
23 July 2011Dear Bala:
I am writing to invite you to attend the next meeting of the Gravitational Wave International Committee (GWIC) to present the GWIC membership application for IndIGO. This in-person meeting will give you the opportunity to interact with the members of GWIC and to answer their questions about the status and plans for IndIGO. Jim Hough (the GWIC Chair) and I have reviewed your application and believe that you have made a strong case for membership……
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)]
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
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
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)
Dear Prof. Kasturirangan, 1 June 2011
In its road-map with a thirty year horizon, the Gravitational Wave International Committee (a working unit of the International Union of Pure and Applied Physics, IUPAP) has identified the expansion of the global network of gravitational wave interferometer observatories as a high priority for maximizing the scientific potential of gravitational wave observations. We are writing to you to put forward a concept proposal on behalf of LIGO Laboratory (USA) and the IndIGO Consortium, for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site. In what follows this project is referred to as LIGO-India. The key idea is to utilize the high technology instrument components already fabricated for one of the three Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories.
LIGO-India 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
LIGO-India: Why is it a good idea?for India
• Has a 20 year legacy and wide recognition in the Intl. GW community with seminal contributions to Source modeling (RRI)& Data Analysis (IUCAA). High precision measurements (TIFR), Participation in LHC (RRCAT)
• (Would not make it to the GWIC report, otherwise!)– AIGO/LIGO/EGO strong interest in fostering Indian community– GWIC invitation to IndIGO join as member (July 2011)
• Provides an exciting challenge at an International forefront of experimental science. Can tap and siphon back the extremely good UG students trained in India. (Sole cause of `brain drain’).
– 1st yr summer intern 2010 MIT for PhD– Indian experimental scientist Postdoc at LIGO training for Adv. LIGO subsystem
• Indian experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India.
– Sendhil Raja, RRCAT, Anil Prabhakar, EE, IIT Madras, Pradeep Kumar, EE, IITK Photonics– Vacuum expertise with RRCAT (S.K. Shukla, A.S. Raja Rao) , IPR (S.K. Bhatt, Ajai Kumar)
• Jump start direct participation in GW observations/astronomy – going beyond analysis methodology & theoretical prediction --- to full fledged participation in
experiment, data acquisition, analysis and astronomy results.
• For once, may be perfect time to a launch into a promising field (GW astronomy) with high end technological spinoffs well before it has obviously blossomed. Once in a generation opportunity to host an Unique International Experiment here.
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.
LIGO-India: Salient points
(vis a vis other mega-projects)• On Indian Soil• Historical science discovery participation• Expenditure mostly in Indian labs & Industry• International Cooperation, not competition• Shared science risk with Intl. community• Initial setup risks, troubleshooting rests with
Advance LIGO USA• Well defined training possibility at advance LIGO
USA installation and commissioning for Indian technical team
• Related major data analysis centre with huge University secto involvement.
Network HHLV HILV AHLV
Mean horizon distance
1.74 1.57 1.69
Detection Volume
8.98 8.77 8.93
Volume Filling factor
41.00% 54.00% 44.00%
Triple Detection Rate(80%)
4.86 5.95 6.06
Triple Detection Rate(95%)
7.81 8.13 8.28
Sky Coverage: 81%
47.30% 79.00% 53.50%
Directional Precision
0.66 2.02 3.01
Strategic geographical relocation comparison
LIGO-India: … the opportunity
Strategic Geographical relocation
Source localization error
5-15 degrees to ~degree !!!
Ellipses version as in LIGO-Aus proposal ?
LIGO-India: … the opportunityStrategic Geographical relocation
Polarization info
Sky coverage ?
LIGO-India: … the opportunity
Strategic Geographical relocation- the science gain
Sky coverage: Synthesized Network beam(antenna power)
LIGO-India: … the opportunity
Strategic Geographical relocation- the science gain
Sky coverage: ‘reach’ /sensitivity in different directions
LIGO-India: unique once-in-a-generation opportunity
LIGO-Lab contribution to LIGO-India• 180 W pre-stablized Nd:YAG laser
• Input condition optics, including electro-optic modulators, Faraday isolators, a suspended mode-cleaner (12-m long mode-defining cavity), and suspended mode-matching telescope optics.
• five "BSC chamber" seismic isolation systems (two stage, six degree of freedom, active isolation stages capable of ~200 kg payloads)
• six "HAM Chamber" seismic isolation systems (one stage, six degree of freedom, active isolation stages capable of ~200 kg payloads)
• eleven Hydraulic External Pre-Isolation systems (mount external to chamber for longer range and lower frequency isolation and actuation
• 10 interferometer core optics (test masses, folding mirrors, beam splitter, recycling mirrors)
LIGO-Lab contribution to LIGO-India
* Five quadruple stage large optics suspensions systems
* Triple stage suspensions for remaining suspended optics
* Baffles and beam dumps for controlling scattering and stray radiation
* Optical distortion monitors and thermal control/compensation system for large optics
* Photo-detectors, conditioning electronics, actuation electronics and conditioning
* Data conditioning and acquisition system, software for data acquisition
* Supervisory control and monitoring system, software for all control systems
* Installation tooling and fixturing
LIGO-India: unique once-in-a-generation opportunity
LIGO-India: Indian Contributions
• Indian contribution in infrastructure : Site Vacuum systemRelated ControlsData centre Trained manpower for installation and
commissioning Trained manpower for LIGO-India operations for
10 years
LIGO-India vs future IndianIGO : Major Advantages
• Cutting edge instrument to jump start GW astronomy. Would require at least a decade of focused technology development to get there
• 180 W Nd-Yag: 5 years; Rs. 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 forisolation 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 ofdedicated 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.
The Science Payoffs• New Astronomy, New Astrophysics, New Cosmology, New
Physics…A New Window ushers a New Era of Exploration• Testing Einstein’s GR in strong and time-varying fields• Testing Black Hole phenomena• Understanding nuclear matter by Neutron star EOS• Neutron star coalescence events• Understanding most energetic events in the
universe..Supernovae, Gamma-ray bursts, LMXB’s, Magnetars• New cosmology..SMBHB’s as standard sirens..EOS of Dark
Energy• Multi-messenger astronomy• The Unexpected
The Technology Payoffs• Lasers and optics..Purest laser light..Low phase noise,
excellent beam quality, high single frequency power• Applications in precision metrology, medicine, micro-
machining• Coherent laser radar and strain sensors for earthquake
prediction and other precision metrology• Surface accuracy of mirrors 100 times better than telescope
mirrors..Ultra-high reflective coatings• Vibration Isolation and suspension..Applications for mineral
prospecting• Squeezing and quantum limits• Ultra-high vacuum system 10^-9 torr..Largest in the region• Computation Challenges; Cloud computing, new hardware
and software tools for computational innovation
The rewards and spinoffs• Detection of GW is the very epitome of breakthrough science.• In collaborating with USA to realize LIGO-India, India could
become a partner in international science of Nobel Prize significance
• GW detection is an instrument technology intensive field pushing frontiers simultaneously in a number of fields like lasers and photonics. Impact allied areas and smart industries.
• The imperative need to work closely with industry and other end users will lead to spinoffs as GW scientists further develop optical sensor technology.
• Presence of LIGO-India will lead to pushing technologies and greater innovation in the future.
• The largest UHV system will provide industry a challenge and experience.
…The rewards and spinoffs• LIGO-India can raise profile of science since it will be making
ongoing discoveries fascinating the young. GR, BH, EU and Einstein has a special attraction and a pioneering facility in India participating in important discoveries will provide role models with high visibility and media interest.
• LIGO has a strong outreach tradition and LIGO-India will provide a platform to increase it and synergically benefit.
• Increase number of research groups performing at world class levels and produce skilled researchers.
• Increase number of businesses investing in R&D. Provide opportunities to increase proportion of industries engaging in innovation.
• Increase international collaborations in Indian research. Science Leadership in the Asia-Pacific(?) region
LIGO-India: … the challenges Organizational
National level DST-DAE Consortium Flagship Mega-project Identify a lead institution and agency Project leaderConstruction: 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 specsTrain 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
LIGO-India: … the challenges
Trained Manpower for installation & commissioning
LIGO-India DirectorProject managerProject engineering staff: Civil engineer(s)Vacuum engineer(s)Systems engineer(s),Mechanical engineersElectronics engineersSoftware engineers Detector leaderProject system engineerDetector 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)]
Logistics and Work Plan• Assumption: Project taken up by DAE as a National Mega
Flagship Project. All the persons mentioned who are currently working in their centers would be mainly in a supervisory role of working on the project during the installation phase and training manpower recruited under the project who would then transition into the operating staff.
• Instrument Engineering: No manpower required for design and development activity. For installation and commissioning phase and subsequent operation
• Laser ITF: Unnikrishnan, Sendhil Raja, Anil Prabhaker. TIFR, RRCAT, IITM. 10 Post-doc/Ph.D students. Over 2-3 years. Spend a year at Advanced LIGO. 6 full time engineers and
scientists. If project sanctioned, manpower sanctioned, hirings possible at RRCAT.. TIFR??
Large scale ultra-high Vacuum enclosureS.K. Shukla (RRCAT),A.S. Raja Rao (ex RRCAT),
S. Bhatt (IPR), Ajai Kumar (IPR)• To be fabricated by IndIGO with designs from LIGO. A pumped
volume of 10000m3 (10Mega-litres), evacuated to an ultra high vacuum of 10-9 torr.
• Spiral welded beam tubes 1.2m in diameter and 20m length. • Butt welding of 20m tubes together to 200m length. • Butt welding of expansion bellows between 200m tubes.• Gate valves of 1m aperture at the 4km tube ends and the
middle.• Optics tanks, to house the end mirrors and beam
splitter/power and signal recycling optics vacuum pumps.• Gate valves and peripheral vacuum components. • Baking and leak checking
• 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
Large scale ultra-high Vacuum enclosure
Logistics and Work Plan• Clean rooms: Movable tent type clean rooms during welding of the beam
tubes and assembly of the system. Final building a clean room with AC and pressurization modules. SAC, ISRO. 1 engineer and 2 technicians to draw specs for the clean room equipments and installation.
• Vibration isolation system: 2 engineers (precision mechanical) to install and maintain the system. Sourced from BARC. RED (Reactor Engineering Division of BARC) has a group that works on vibration measurement, analysis and control in reactors and turbo machinery.
• Electronic Control System: 4 Engineers to install and maintain the electronics control and data acquisition system. Electronics & Instrumentation Group at BARC (G. P. Shrivastava’s group) and RRCAT. Preliminary training:six months at LIGO. Primary responsibility (installing and running the electronics control and data acquisition system): RRCAT & BARC. Additional activity for LIGO-India can be factored in XII plan if the approvals come in early.
Logistics and Work Plan• Understand teams at Electronics & Instrumentation Group at BARC looking
for large instrumentation projects in XII plan.• Control software Interface: 2 Engineers (install and maintain the computer
software interface, distributed networking and control system). RRCAT and BARC. Computer software interface (part of the data acquisition system) and is the “Human-machine-interface” for the interferometer. For seamless implementation man power to be sourced from teams implementing Electronic Control System.
• Site Selection & Civil Constructions: BARC Seismology Division Data reg. seismic noise at various DAE sites to do initial selection of sites and shortlist based on other considerations such as accessibility and remoteness from road traffic etc. DAE: Directorate of Construction, services and Estate Management (DCSEM): Co-ordinate design and construction of the required civil structures required for the ITF. 2 engineers + 3 technicians (design & supervision of constructions at site). Construction contracted to private construction firm under supervision of DCSEM.
• 42 persons (10 PhD/postdocs, 22 scientists/engineers and 10 technicians)
LIGO-India: … the challenges
Manpower generation for sustenance of the LIGO-India observatory : Plans & Preliminary exploration• Since Advanced LIGO will have a lead time, participants will be identified
who will be deputed to take part in the commissioning of Advanced LIGO and later bring in the experience to LIGO-India
• Successful Summer internships in International labs underway.. Plan to extend to National labs to generate more experimenters• IndIGO schools are planned annually to expose students to emerging
opportunities and attract some to join.• Post graduate school specialization course• Jayant Narlikar: Since sophisticated technology is involved IndIGO should
like ISRO or BARC training school set up a program where after successful completion of the training, jobs are assured.
LIGO-India: … the challengesIndian SiteRequirements:
Low seismicityLow human generated noiseAir 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• •
LIGO-India: Action pointsIf accepted as a National Flagship Mega Project under
the 12th plan then…• Seed Money• Identification of 3-6 project leaders• Detailed Project Proposal • Site identification• 1st Staffing Requirement meeting Aug 1-15• 2nd Joint Staffing Meeting with LIGO-Lab• Vacuum Task related team and plans
Concluding remarks• A century after Einstein predicted them, and after four
decades of very innovative and Herculean struggle, We are on the threshold of a new era in GW detection.
• First generation detectors like Initial LIGO and Virgo have reached design sensitivity . Have broken new ground in optical sensitivity, pushed technology and proved the technique.
• Second generation detectors are starting installation and expected to expand the “Science” by factor of 1000
• A worldwide network is starting to come on line and the ground work has been laid for operation as a integrated system.
• An unique once-in-a-generation opportunity for India. India could play a key role by hosting LIGO-India.
• A compelling Science case, a proven design. Need strong institutional support to bring together capable participants.
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 Req Doc of LIGO-Lab will need to be ready for LIGO-Lab examination latest by Dec 2011 so that in turn LIGO-Lab can make a case with NSF by Jan 2012.
• Of all the large scientific projects out there, this one is pushing the greatest number of technologies the hardest.
“Every single technology they’re touching they’re pushing, and there’s a lot of different technologies they’re touching.”
(Beverly Berger, National Science Foundation Program director for gravitational physics. )
• One is left speculating if by the centenary of General Relativity in 2015, the first discovery of Gravitational waves would be from a Binary Black Hole system and Chandrasekhar would be doubly right about Astronomy being the natural home of general relativity.
THE END
The IndIGO data analysis centre• Tier -2 centre with data archival
and computational facilities• Inter-institutional proposal for
facility• Propose for a high-throughput
Computation and GW Data Archival Centre.
• Will provide fundamental infrastructure for consolidating GW data analysis expertise in India.
Tier 0 •LIGO Sites at Hanford, Livingston •Data acquisition systems
Tier 1 •LIGO Labs at Caltech
Tier 2 •LIGO Lab at MIT, LSC institutions like UWM, Syracuse etc•IndIGO Data Analysis Centre
Courtesy: Anand Sengupta
Objectives of the data centre
Tier 2Data
Centreat
IUCAA
Archiva
l
LIGO Data Grid as a role model for the proposedIndIGO Data Analysis Centre.
Courtesy: Anand Sengupta
LIGO-India
Future GWDA Plans of IndIGO (as part of LSC)
Project leads: Sanjit Mitra, T. Souradeep, S. Dhurandhar …
Extend GW radiometer work (Mitra,Dhurandhar, TS,…2009) Implementation of the cross-correlation search for
periodic sources (Dhurandhar + collab.)
Burst Sources • Formulation• Implementation
Courtesy: S. Dhurandhar
Vetoes for non-Gaussian noise for coherent detection of inspirals
• Project leads: Anand Sengupta, Archana Pai, M K Harris.
Non-Gaussian noise plagues the detector data
Vetoes have been developed in LSC for removal of non-Gaussian noise in the single detector case
For coincidence search the veto is obvious but for coherent not so.
Developing a veto for coherent is crucial – chi squared
Scope for improving the current chi squared test – Japanese collaboration
8th February Delhi Courtesy: S. Dhurandhar
Tests of General Relativity using GW observations
Project leads: K G Arun, Rajesh Nayak and Chandra Kant Mishra, Bala Iyer
GWs are unique probes of strong field gravity. Their direct detection would enable very precise tests of GR in the dynamical and strong field regime.
Preparing data analysis algorithms for AdvLIGO in order to test GR and its alternatives is one of the important and immediate goals of LSC.
Plan to take part in the activity to develop parameter estimation tools based on Bayesian methods.
Possible collaboration with B S Sathyaprakash (Cardiff University) & P Ajith (Caltech).
Courtesy: S. Dhurandhar
Indo-Aus.Meeting, Delhi, Feb 2011
Detector subsystem leaders: approximately 10 talented scientists or researchengineers with interest and knowledge collectively spanning: Lasers and optical devices Optical metrology, handling and cleaning Precision mechanical structures Low noise electronics Digital control systems and electro-mechanical servo design Vacuum cleaning and handling
We will easily be able to find, train and commit people in 4 areas:lasers and optical devices, optical metrology, low noise electronics,digital control and electro-mechanical servo design
Precision mechanical structures and vaccuum systems is also possible,but I would have to talk to other faculty.
I say find, train and commit, because we don't have too manyscientific staff in the institute. The modus operandi would be tostart off with project staff, who are working towards a degree andhence are committed for 3-4 years, and who can then be absorbed intoLIGO-India. An alternative way is to sponsor the degree directly (wejust started a program for Texas Instr, where students get a 50%higher stipend, work only on TI projects, and are guaranteed jobs atTI). Numbers won't be a problem, if there is demand. Our presentannual intake in optics is around 15, so identifying 3-5 is easyenough. We always have tons of applicants for our programs, butquality is a bit spotty, so training becomes important.
The higher level positions at project system engineer, detector leaderand project engineering staff, should be hired for pay, comparable toany large engineering project. People are there.....it is just thatsomeone like HCL or GE, forks out 8-10 lakhs/year for one of our freshMaster's students. So, if LIGO-India pays, they will join.
Change in Length manifests as Change in Transmitted Light
GW detection is about seeing the biggest things that ever happen by measuring the smallest changes that have ever been measured - Harry Collins.
Laser Interferometer GW Observatory
4 km: 1.2m diameter high vaccum tubesIndia
180 W(Germany)
Seismic isolation
Stacks (GEO, U
K)
Optics & controls(USA)
40 kgFused silica
mirrors(USA)
Fig from LIGO-AUS report?
If retained get better res picture
Era of Advanced LIGO detectors: 2015
Courtesy: B. Schutz: GWIC Roadmap Document
GWIC: Gravitational Wave International Committee
LIGO-Australia: Idea and Opportunity
• The NSF approved grand decision to locate one of the planned LIGO-USA interferometer detector at Gingin site, W. Australia to maximize science benefits like baseline, pointing, duty cycle, technology development and international collaboration.
• The proposal from Australian consortium envisages IndIGO as one of the partners to realize this amazing opportunity.
- Indian contribution in hardware (end station vacuum system, and controls), Data centre, manpower for installation and commissioning.
LIGO-India: … the opportunity
Strategic Geographical relocation
Network: HIJLV GMRT BangaloreMean horizon distance: 1.57 1.63Detection Volume: 12.0 12.0Volume Filling factor: 73% 66%Triple Detection Rate(80%): 8.62 8.64Triple Detection Rate(95%): 11.1 11.1Sky Coverage: 100% 100%Directional Precision: 2.93 3.00
Figure?
LIGO-India: … the Opportunity
• Part of a fundamental scientific discovery : direct detection of gravitational radiation
• Part of “historic” launch of a new window of Astronomy• LIGO-India: Southernmost, hence, Unique role in the
Intl. GW observatory network.
• Full detector at about half the cost is the naïve calculation.
Adv. LIGO detector system is worth 15 years of challenging R &D – price tag?
• Indian Labs & Industry • •
LIGO-India: … the challengesInternational competition
Issues:
Preliminary assessment:
LIGO-India: … the challengesShort lead time
Requirements:
Preliminary exploration: