IndIGOIndian Initiative in Gravitational-wave Observations
Detecting Einstein’s Elusive Waves
Opening a New Window to the Universe Inaugurating Gravitational wave
AstronomyLIGO-India: An Indo-US joint mega-project concept proposal Bala Iyer, RRI, BangaloreBala Iyer, RRI, Bangalore
Chair, IndIGO Consortium CouncilChair, IndIGO Consortium CouncilOn behalf of the IndIGO ConsortiumOn behalf of the IndIGO Consortium
Version: pI_v3 Jun 22, 2011 : BIwww.gw-indigo.org
What are Gravitational waves and how best to detect them??
Beauty & Precision
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 SR will lead to GW…However, the properties of GW in different theories of gravity
could be different …
PPulsar
Companion NS
1975 - Hulse and Taylor Binary Pulsar 1913+16
•Exquisite Lab for Tests of GR beyond static & weak Grav fields •High quality Pulsar Timing Data shows that after correcting for ALL known relativistic and astrophysical kinematic effects, the binary system is losing orbital energy •Period (measurable to 50ms accuracy) speeds up by 14s from 1975-94 as predicted by Einstein’s GR. Binary pulsar systems emit gravitational waves Nobel Prize clinching evidence for Gravitational Nobel Prize clinching evidence for Gravitational
waves BUT still waves BUT still IndirectIndirect evidence…. evidence….
Nobel prizein 1993 !!!
Courtesy;: Stan
Whitcomb
6
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
GW cause Oscillatory Tidal distortions on a ring of particles GW cause Oscillatory Tidal distortions on a ring of particles
•Path difference due to tidal distortion phase difference •Change in Length manifests as a Change in Transmitted Light
LLh /Strain
Suspended mirrors of an interferometer act as (freely falling) test masses Suspended mirrors of an interferometer act as (freely falling) test masses (in hor pl for f>>f_pend),undergo tidal deformations leading to path differences(in hor pl for f>>f_pend),undergo tidal deformations leading to path differences
Challenge of GW Detection A century of waiting
• Two Fundamental Diffs between GR &EM- Weakness of Gravitation relative to EM (10^-39)
-Massless Spin two nature of Gravitation vs Spin one of EM that forbids dipole radiation in GR
• A NS-NS Binary in the Virgo cluster (20 Mpc) produces a strain of h ~ 10–22 – 10–21 .
• For a 4 km detector one must effectively measure the miniscule displmnt L ~ 10-18 m
• GW detection is about seeing the biggest GW detection is about seeing the biggest things that ever happen by measuring the things that ever happen by measuring the smallest changes that have ever been smallest changes that have ever been measured - Harry Collins.measured - Harry Collins.
Courtesy: Stan Whitcomb
end test mass
beam splittersignal
LIGO Optical Configuration
Laser
MichelsonInterferometer
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
Detecting GW with Laser Interferometer
Difference in distance of Paths Interference of laser light at the detector (Photodiode)
Current Status of World-wide GW detection efforts
IndIGO - ACIGA meeting 11
Laser Interferometer Gravitational-wave Observatory (LIGO) USA, 4 km
Virgo (Cascina, near Pisa, Italy) French-Italian, 3km
Experimental Milestone Km-scale interferometric GW detectors LIGO and Virgo achieved their predicted design goals. Strain sensitivity <3x10-23/Sqrt(Hz) at 200 Hz.
Unprecedented sensitivity already allows• Upper Limits on GW from a variety of Astrophysical sources. • Improve on Spin down of Crab, Vela pulsars.. Less than 2% available energy in Crab emitted as GW• Surpass Big Bang nucleosynthesis bound on Stochastic GW.. Pre-dawn GW astronomy
Towards Advanced LIGO & Virgo
Era of Advanced LIGO detectors: 2015
10x sensitivity10x dist reach 1000 volume
>> 1000X event rate
(reach beyond
nearest super-clusters)
A Day of Advanced LIGO Observation >> A year of Initial LIGO
observation
Mean Expected Annual Coalescence Event Rates
Detector Generation
NS-NS NS-BH BH-BH
Initial LIGO(2002 -2006) 0.02 0.0006 0.0009
Advanced LIGO(10X sensitivity)(2014+ - …)
40 10. 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 rateestimates, Population Synthesis models. Rates quoted below are mean of the distribution.
Need for Long baseline global Network:
IndIGO opportunities and benefits
18
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..”
•Aside: Invitation to Present on July 10 during GWIC Meeting at Aside: Invitation to Present on July 10 during GWIC Meeting at Amaldi9 in Cardiff the IndIGO case for GWIC Membership Amaldi9 in Cardiff the IndIGO case for GWIC Membership
Members: All major GW Detector groups
Global Network of GW Observatories improves…Global Network of GW Observatories improves…
LIGO-LLO: 4km
LIGO-LHO: 2km+ 4kmGEO: 0.6km VIRGO: 3km
LCGT 3 kmTAMA/CLIO
LIGO-Australia?
1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info.
LIGO-India ?
LIGO-India: … the opportunityScience Gain from Strategic Geographical Relocation
Source localization error
Original Plan 2 +1 LIGO USA+ Virgo
LIGO-India plan1+1 LIGO USA+ Virgo+ LIGO-India
LIGO-Aus plan1+1 LIGO USA+ Virgo+ LIGO-Aus
Courtesy:S. Fairhurst
Gravitational wave legacy in India• Indian contribution over two decades, to the global effort for
detecting GW, internationally recognized on two significant fronts• Seminal contributions to source modeling at RRI [Bala Iyer] and to
GW data analysis at IUCAA [Sanjeev Dhurandhar]• RRI: Indo-French collaboration for two decades to compute high accuracy
waveforms for in-spiraling compact binaries from which the GW templates used in LIGO and Virgo are constructed.
• IUCAA: Designing efficient data analysis algorithms involving advanced mathematical concepts.. Notable contributions include the search for binary in-spirals, hierarchical methods, coherent search with a network of detectors and the radiometric search for stochastic gravitational waves.
• IUCAA has collaborated with most international GW detector groups and has been a member of the LIGO Scientific Collaboration (LSC) for a decade.
• At IUCAA, Tarun Souradeep with expertise in CMB data and Planck has worked to create a bridge between CMB and GW data analysis challenges.
Indian Gravitational wave community strengths
• Very good students and post-docs produced who are… * Leaders in GW research abroad [Sathyaprakash, Bose, Mohanty] (3)
*New faculty at premier institutions in India (6) [Gopakumar, Archana Pai, Rajesh Nayak, Anand Sengupta, K.G. Arun, Sanjit Mitra, P. Ajith?]
• Strong Indian presence in GW Astronomy in the Global Strong Indian presence in GW Astronomy in the Global detector network detector network where broad international collaboration is the norm where broad international collaboration is the norm
relatively easy to get well trained researchers back relatively easy to get well trained researchers back
• Close interactions with Rana Adhikari (Caltech), B.S. Sathyaprakash (Cardiff), Sukanta Bose ( WU, Pullman), Soumya Mohanty (UTB), Badri Krishnan ( AEI) …
• Very supportive International community as reflected in the International Advisory committee of IndIGO – Chair Abhay Ashtekar
• LIGO-Lab participation in IndIGO schools, commitment to training and assisting in high end technology tasks
• EGO proposal to explore MoU for GW collaboration: Roadmap Meeting on Nov 1-2 ,2011 at IUCAA
High precision Expertise in India• TIFR [C.S. Unnikrishnan] : High precision experiments and tests of weak forces
– 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 expt./AdvLIGO)
• 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..
• RRCAT – [S.K. Shukla on INDUS, A.S. Raja Rao (exRRCAT)] --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….
Large experiment expertise in India
• RRCAT….• IPR [S.B. Bhatt on Aditya and Ajai Kumar] - UHV experience, Lasers…
Support role in large volume UHV system, Control systems etc
• 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.
• Teams at Electronics & Instrumentation Groups at BARC (may be interested in large instrumentation projects in XII plan)
• Groups at ISRO,…….
Multi-Institutional,Multi-disciplinary Consortium(2009)
1. CMI, Chennai2. Delhi University3. IISER Kolkata4. IISER Trivandrum5. IIT Madras (EE)6. IIT Kanpur (EE)7. IUCAA, Pune8. RRCAT, Indore9. TIFR, Mumbai10. IPR, Bhatt
Others• RRI• Jamia Milia Islamia• Tezpur Univ
Nodal InstitutionsNodal Institutions
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. Sanjay Sahay BITS, Goa16. P Ajith Caltech , USA17. Sukanta Bose, Wash. U., USA18. B. S. Sathyaprakash Cardiff University, UK19. Soumya Mohanty UTB, Brownsville , USA20. 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. Bhal Chandra Joshi NCRA, Pune13. Rijuparna Chakraborty, Cote d’Azur, Grasse14. Rana Adhikari Caltech, USA 15. Suresh Doravari Caltech, USA 16. 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
IndIGO: the goals & roles - I
• Provide a common umbrella to initiate and expand GW related experimental activity and train new technically skilled 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,…
• Seek 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
• Start collaborative work on joint projects under the IUSSTF Indo-US IUCAA-Caltech joint Centre at IUCAA
IndIGO 3m Prototype Detector
Funded by TIFR Mumbai on campus (2010)PI: C. S.Unnikrishnan (Cost ~ INR 2.5cr) Technology Development and Training Platform
Vacuum tanksDetector
Laser table
Vibration isolationschematic
All mirros and beamsplitters are suspended as in the diagram on right
3.2 meters
0.8 mF-P cavityPower recycling
Sensing &Control
60 cm
180 cm
Mirror
IndIGO: the goals & roles - II• Set up a major experimental initiative in GW astronomy
MOU with ACIGA to collaborate on GW AstronomyEarlier 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 with offer of LIGO-India and Requirement Document– Advanced LIGO hardware for 1 detector to be shipped to India.– Two 4km arm length ultra high vacuum tubes in L configuration– India provides suitable site and infrastructure to house the GW observatory, Staffing for
installing, commissioning and operation and 10 year Running costs– Indian cost ~ Rs 1000Cr
The Science & technology benefit of LIGO-India is transformational
LIGO-India: Why is it a good idea?… for the World
• Geographical relocation Strategic for GW astronomy– Increased event rates (x4) 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
LIGO-India: Why is it a good idea?
• Jump start direct participation in GW Observations & Astronomy • Provides an exciting challenge at the International forefront of
experimental science. Can tap and siphon back the extremely good UG students trained in India. (a cause for `brain drain’).
– 1st yr summer intern 2010 MIT for PhD– Indian experimental scientist Postdoc at LIGO training for Adv. LIGO
subsystem; Another Postdoc under consideration in LIGO & EGO
• Experimental expertise related to GW observatories will thrive and attain high levels due to LIGO-India.
• Challenging endeavour involving unforgiving technology mandates symbiotic interplay of Engineering and Science disciplines.. Revival of Advanced Instrumentation
• Inclusive cooperation between Basic science research Institutes, High Technology DAE Labs, ISRO,..Educational IISER’s and Universities for highly visible frontier research
……..for India
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 !
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• •
Summary (Part 1)
• LIGO-India will raise public profile of science since it will be making ongoing discoveries fascinating the young.
GR, BH, EU and Einstein have a special attraction and a pioneering facility in India participating in important discoveries will provide science & technology role models with high visibility
and media interest. Einstein@home; Black Hole Hunter…
• Opportune to a launch a promising field (GW astronomy) with high end technological spinoffs, well before it has obviously blossomed. Once in a generation unique Once in a generation unique opportunity to host in India a sophisticated International opportunity to host in India a sophisticated International Experiment straining to hear the feeble notes of Einstein’s Experiment straining to hear the feeble notes of Einstein’s GW Symphony playing in the universe and deciphering the GW Symphony playing in the universe and deciphering the dark secrets that light or EMW can never reveal.. dark secrets that light or EMW can never reveal..
• A GREAT opportunity but a very sharp deadline of 31 Mar 2012. • LIGO-Lab needs to seek NSF nod latest by Dec 2011
– We must be ready with credible plan proposal from We must be ready with credible plan proposal from India by Nov 2011India by Nov 2011
Thank you !!!Thank you !!!
Over to Tarun…Over to Tarun…
End of Part IEnd of Part I
Committees: National Steering Committee:Kailash Rustagi (IIT, Mumbai) [Chair]Bala Iyer (RRI) [Coordinator]Sanjeev Dhurandhar (IUCAA) [Co-Coordinator]D.D. Bhawalkar (Quantalase, Indore)[Advisor]P.K. Kaw (IPR)Ajit Kembhavi (IUCAA) P.D. Gupta (RRCAT)J.V. Narlikar (IUCAA)G. Srinivasan
International Advisory Committee
Abhay Ashtekar (Penn SU)[ Chair]Rana Adhikari (LIGO, Caltech, USA)David Blair (ACIGA &UWA, Australia)Adalberto Giazotto (Virgo, Italy)P.D. Gupta (Director, RRCAT, India)James Hough (GEO ; Glasgow, UK)[GWIC Chair]Kazuaki Kuroda (LCGT, Japan)Harald Lueck (GEO, Germany)Nary Man (Virgo, France)Jay Marx (LIGO, Director, USA)David McClelland (ACIGA&ANU, Australia)Jesper Munch (Chair, ACIGA, Australia)B.S. Sathyaprakash (GEO, Cardiff Univ, UK)Bernard F. Schutz (GEO, Director AEI, Germany)Jean-Yves Vinet (Virgo, France)Stan Whitcomb (LIGO, Caltech, USA)
IndIGO Advisory Structure
Program Management Committee:C S Unnikrishnan (TIFR, Mumbai), [Chair]Bala R Iyer (RRI, Bangalore), [Coordinator]Sanjeev Dhurandhar (IUCAA, Pune) [Co-cordinator]Tarun Souradeep (IUCAA, Pune)Bhal Chandra Joshi (NCRA, Pune)P Sreekumar (ISAC, Bangalore)P K Gupta (RRCAT, Indore)S K Shukla (RRCAT, Indore)Sendhil Raja (RRCAT, Indore)]
LIGO-India: … the opportunity
Polarization info
Homogeneity of Sky coverage
Courtesy: S.Kilmenko & G. Vedovato
Strategic Geographical relocation: science gain
LIGO-India: … the opportunity
Sky coverage: Synthesized Network beam(antenna power)
Courtesy: B. Schutz
Strategic Geographical relocation: science gain
LIGO-India: … the opportunity
Sky coverage: ‘reach’ /sensitivity in different directions
Courtesy: B. Schutz
Strategic Geographical relocation: science gain
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: science gain
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.
vit
GWIC Roadmap Document
Gravitational wave Astronomy :
Unique Technology Payoffs• Lasers and optics..Purest laser light..Low phase noise, excellent
beam quality, high single frequency power• Applications in precision metrology, medicine, micro-machining• Coherent laser radar and strain sensors for earthquake prediction
and other precision metrology• Surface accuracy of mirrors 100 times better than telescope
mirrors..Ultra-high reflective coatings : New technology for other fields
• Vibration Isolation and suspension..Applications for mineral prospecting
• Squeezing and challenging “quantum limits” in measurements.• Largest Ultra-high vacuum system 10^-9 torr (1picomHg) in the
region. Such a UHV system will provide industry a challenge and experience.
• Computation Challenges: Cloud computing, Grid computing, new hardware and software tools for computational innovation.
vit
GWIC Roadmap Document
Gravitational wave Astronomy :
Synergy with other major Astronomy projects
• SKA : Pulsars timing and GW background, GW from Pulsars ,…( RADIO: Square Kilometer array)• CMB : GW from inflation, cosmic phase transitions, dark energy ….(Cosmic Microwave Background : WMAP, Planck, CMBPOl, QUaD,…)• X-ray satellite (AstroSat) : Spacetime near Black Holes, NS, …. • Gamma ray observatory: GRB triggers from GW(FermiLAT, GLAST,….)• Thirty Meter Telescope: Resolving multiple AGNs, optical follow-up, …• INO: cross correlate neutrino signals from SN event• LSST: Astro-transients with GW triggers, Cosmic distribution of dark matter , Dark energy• •
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 to present the GWIC membership application for IndIGO.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 you have made a strong case for membership……membership……
Invitation to Present IndIGO case for GWIC Membership on July 10 at GWIC meeting at Cardiff
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 path” in the curved space-time caused by sun’s mass !!!
What happens when
matter is in motion?
Detecting GW with Laser Interferometer
Difference in distance of Path A & B Interference of laser light at the detector (Photodiode)
Path A
Path B
AB
Indo-Aus.Meeting, Delhi, Feb 2011
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.
… 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 Astronomy being the natural home of general relativity.relativity.
52
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
Advanced LIGO•Take advantage of new technologies and on-going R&D
>> Active anti-seismic system operating to lower frequencies:(Stanford, LIGO)
>> Lower thermal noise suspensions and optics : (GEO )
>> Higher laser power 10 W 180 W (Hannover group, Germany)
>> More sensitive and more flexible optical configuration: Signal recycling
• Design: 1999 – 2010 : 10 years of high end R & D internationally.
• Construction: Start 2008; Installation 2011; Completion 2015
A Century of Waiting• Almost 100 years since Einstein predicted GW but
no direct experimental confirmation (a la Hertz for Maxwell EM theory)
• Two Fundamental Difference between GR and EM- Weakness of Gravitation relative to EM (10^-39)-Spin two nature of Gravitation vs Spin one of EM that forbids dipole
radiation in GR
• Low efficiency for conversion of mechanical energy to GW & Feeble effects of GW on any Detector
• GW Hertz experiment ruled out. Only astrophysical systems involving huge masses and accelerating very strongly are potential detectable sources of GW signals.
Astrophysical systems are sources of copious GW emission:
•GW emission efficiency (10% of mass for BH mergers) >> EM radiation via Nuclear fusion (0.05% of mass)
Energy/mass emitted in GW from binary >> EM radiation in the lifetime
• Universe is buzzing with GW signals from cores of astrophysical 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
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
Principle behind Detection of GW Principle behind Detection of GW
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 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 Consortium, for a Joint Partnership venture to set up an Advanced gravitational wave detector at a suitable Indian site. at a suitable Indian site. In what follows this project is referred to as LIGO-India. The key idea The key idea is to utilize the high technology instrument components already fabricated for one of the three 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 Advanced LIGO interferometers in an infrastructure provided by India that matches that of the US Advanced LIGO observatories.US Advanced LIGO observatories.
LIGO-India could be operational early in the lifetime of the advanced versions of gravitational wave operational early in the lifetime of the advanced versions of gravitational wave observatoriesobservatories 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 India would be unique among nations leading the scientific exploration of this new window on the universeof this new window on the universe. The present proposal promises to achieve this at a fraction of a fraction of the total cost of independently establishing a fully-equipped and advanced observatory. 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 from LIGO
Pulsar companion
Binary Pulsars..NS-NS Binary
High quality observational data that GW exist….
Indian Gravitational wave strengths• Very good students and post-docs produced from this. * Leaders in GW research abroad [Sathyaprakash, Bose, Mohanty] (3) *
*New faculty at premier Indian institutions (6) [Gopakumar, Archana Pai, Rajesh Nayak, Anand Sengupta, K.G. Arun, Sanjit Mitra, P. Ajith?]
– Gopakumar (Jena TIFR) and Arun (Virgo CMI) : PN modeling, dynamics of CB, Ap and cosmological implications of parameter estimation
– Rajesh Nayak (UTB IISER K) , Archana Pai (AEI IISER T), Anand Sengupta (LIGO, Caltech Delhi), Sanjit Mitra (JPL IUCAA ): Extensive experience on single and multi-detector detection, hierarchical techniques, noise characterization schemes, veto techniques for GW transients, bursts, continuous and stochastic sources, radiometric methods, …
– P. Ajith (Caltech, LIGO/TAPIR ? ) ……
– Sukanta Bose (Faculty UW, USA ?)
Strong Indian presence in GW Astronomy with Global detector network Strong Indian presence in GW Astronomy with Global detector network
broad international collaboration is the norm broad international collaboration is the norm
relatively easy to get people back.relatively easy to get people back.• Close interactions with Rana Adhikari (Caltech), B.S. Sathyaprakash (Cardiff),
Sukanta Bose ( WU, Pullman), Soumya Mohanty (UTB), Badri Krishnan ( AEI) …
• Very supportive International community reflected in International Advisory committee of IndIGO – Chair Abhay Ashtekar
• EGO-IndIGO meeting on Nov 1-2 ,2011 at IUCAA to explore collaboration
LIGO-India: Why is it a good idea?
• Provides an exciting challenge at an International forefront of experimental science. Can tap and siphon back the extremely good UG students trained in India. (a cause for `brain drain’). – 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.
• Symbiotic interplay of Engineering and Science disciplines for a challenging endeavour involving unforgiving technology
• Jump start direct participation in GW Observations & Astronomy
……..for India
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• •
LIGO-India: Why is it a good idea?
• Provides an exciting challenge at an International forefront of experimental science. Can tap and siphon back the extremely good UG students trained in India. (a cause for `brain drain’). – 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.
• Symbiotic interplay of Engineering and Science disciplines for a challenging endeavour involving unforgiving technology
• Jump start direct participation in GW Observations & Astronomy
……..for India
• leads to loss of orbital energy
• period speeds up 14 sec from 1975-94
High quality Pulsar Timing Data..• 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 Gravitational wavesIndirect evidence for Gravitational waves
Pulsar
companion
Oscillatory Tidal Effect of GW on a ring of test massesOscillatory Tidal Effect of GW on a ring of test masses
If Interferometer mirrors are the test massesIf Interferometer mirrors are the test masses
•Path difference due to tidal distortion phase difference •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
Rewards and SpinoffsDetection 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. Will impact allied areas and smart industries.
• The imperative need to work closely with industry and other end users will lead to spinoffs as GW scientists further develop optical sensor technology. Presence of LIGO-India will lead to pushing technologies and greater innovation in the future.
• Increase number of research groups performing at world class levels and produce skilled researchers. Increase international collaborations in Indian research & Potential for Indian Science Leadership in the Asia-Pacific region.
• LIGO has a strong outreach tradition and LIGO-India will provide a platform to increase it and synergistically benefit.