Transcript Case for INDIGO

LIGO-India
Detecting Einstein’s Elusive Waves
Opening a New Window to the Universe
An Indo-US joint mega-project concept proposal
IndIGO Consortium
(Indian Initiative in Gravitational-wave Observations)
www.gw-indigo.org
Version: 1Rv2 Jun 19, 2011 : TS
Space Time as a fabric
Special Relativity (SR) replaced Absolute space and Absolute Time by flat 4dimensional 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
Earth follows a “straight path” in the curved
space-time caused by sun’s mass !!!
Beauty & Precision
Einstein’s General theory of
relativity is the most
beautiful, as well as,
theory of modern physics.
It has matched all experimental tests
of Gravitation remarkably well.
Era of precision tests : GP-B,….
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.
GW  Astronomy link
Astrophysical systems are sources of copious GW emission:
•GW emission efficiency (10% of mass for BH mergers) >>
EM radiation via Nuclear fusion (0.05% of mass)
Energy/mass emitted in GW from binary >> EM radiation in the lifetime
• Universe is buzzing with GW signals from cores of astrophysical events
Bursts (SN, GRB), mergers, accretion, stellar cannibalism ,…
• Extremely Weak interaction, hence, has been difficult to detect directly
But also implies GW carry unscreened & uncontaminated signals
GW from Binary Neutron stars
Pulsar
companion
Indirect evidence for Gravity waves
Binary pulsar systems emit gravitational waves
•
leads to loss of orbital
energy
•
period speeds up 14 sec
from 1975-94
•
measured to ~50 msec
accuracy
•
deviation grows
quadratically with time
Nobel prize
in 1993 !!!
Hulse and Taylor
Results for PSR1913+16
Principle behind Detection of GW
Effect of GW on a ring of test masses
Interferometer mirrors as test masses
Detecting GW with Laser Interferometer
LIGO Optical Configuration
Power Recycled
Michelson
Interferometer
end test mass
Light bounces back
and forth along arms
about 100 times
with Fabry-Perot Arm
Cavities
Light is “recycled”
about 50 times
input test mass
Laser
signal
beam splitter
Difference in distance of Paths  Interference
of laser light at the detector (Photodiode)
Courtesy: Stan Whitcomb
Challenge of Direct Detection
Gravitational wave is measured in
terms of strain,
h
(change in length/original length)
2
L
h
L
Gravitational waves are very weak!
Expected amplitude of GW
signals
h  10
Measure changes of
 20
 10
 24
one part in thousand-billion-billion!
Initial LIGO Sensitivity Goal
• Strain sensitivity
<3x10-23 1/Hz1/2
at 200 Hz
l
Sensor Noise
» Photon Shot Noise
» Residual Gas
l
Displacement Noise
» Seismic motion
» Thermal Noise
» Radiation Pressure
15
LIGO and Virgo TODAY
Milestone: Decades-old plans to build and operate large interferometric GW detectors
now realized at several locations worldwide
Experimental prowess: LIGO, VIRGO operating at predicted sensitivity!!!!
Pre-dawn GW astronomy : Unprecedented sensitivity already allows
• Upper Limits on GW from a variety of Astrophysical sources. Refining
theoretical modelling
• Improve on Spin down of Crab, Vela pulsars,
• Exptally surpass Big Bang nucleosynthesis bound on Stochastic GW..
Laser Interferometer Gravitational-wave
Observatory (LIGO)
IndIGO - ACIGA meeting
17
Astrophysical Sources for Terrestrial GW Detectors
• Compact binary inspiral:
– NS-NS, NS-BH, BH-BH
“chirps”
• 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
18
Using GWs to Learn about the Source: an Example
Over two decades,
RRI involved in
computation of
inspiral waveforms
for compact
binaries & their
implications and
IUCAA in its Data
Analysis Aspects.
Can determine
• Distance from the earth r
• Masses of the two bodies
• Orbital eccentricity e and orbital inclination i
Era of Advanced LIGO detectors: 2015
10x sensitivity
10x reach
 1000 volume
>> 1000 event rate
(reach beyond
nearest super-
clusters)
A Day of Advanced
LIGO Observation >>
A year of Initial LIGO
Expected Annual Coalescence Event Rates
Detector
Generation
Initial LIGO
(2002 -2006)
NS-NS
NS-BH
BH-BH
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 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.
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
“Quantum measurements”
to improve further via squeezed light:
• New ground for optical technologists in India
• High Potential to draw the best Indian UG
students typically interested in theoretical
physics into experimental science !!!
Schematic Optical Design of Advanced LIGO detectors
Reflects International cooperation
Basic nature of GW Astronomy
LASER
AEI, Hannover
Germany
Suspension
GEO, UK
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
25
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
Courtesy: Stan Whitcomb
26
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
27
Advanced LIGO Suspensions
• UK designed and contributed
test mass suspensions
• Silicate bonds create quasimonolithic pendulums using
ultra-low loss fused silica fibres
to suspend interferometer optics
– Pendulum
Q ~105 -> ~108
four stages
Suppression at 10 Hz : ?
at 1 Hz : ?
40 kg silica
test mass
Courtesy: Stan Whitcomb
28
28
Scientific Payoffs
Advanced GW network sensitivity needed to observe
GW signals at monthly or even weekly rates.
• Direct detection of GW probes strong field regime of gravitation
 Information about systems in which strong-field and time dependent gravitation
dominates, an untested regime including non-linear self-interactions
• GW detectors will uncover NEW aspects of the physics
 Sources at extreme physical conditions (eg., super nuclear density physics),
relativistic motions, extreme high density, temperature and magnetic fields.
• GW signals propagate un-attenuated
weak but clean signal from cores of astrophysical event where EM signal is
screened by ionized matter.
• Wide range of frequencies  Sensitivity over a range of astrophysical scales
To capitalize one needs a global array of GW antennas separated by
continental distances to pinpoint sources in the sky and extract all the
source information encoded in the GW signals
GW Astronomy with Intl. Network of GW Observatories
1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info.
GEO: 0.6km
LIGO-LHO: 2km+ 4km
VIRGO: 3km
LCGT 3 km
TAMA/CLIO
LIGO-LLO: 4km
LIGO-Australia?
LIGO-India ?
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..
31
Indo-Aus.Meeting, Delhi, Feb
2011
Gravitational wave Astronomy :
vit
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
•
•
GWIC Roadmap Document
The Gravitational wave legacy
Two decades of Indian contribution to the international effort for
detecting GW on two significant fronts :
• Seminal contributions to source modeling at RRI [Bala Iyer] and to GW data
analysis at IUCAA [Sanjeev Dhurandhar] which has been internationally
recognized
• RRI: Indo-French collaboration for two decades to compute high accuracy
waveforms for in-spiraling compact binaries from which the GW templates
used in LIGO and Virgo are constructed.
• IUCAA: Designing efficient data analysis algorithms involving advanced
mathematical concepts.
• Notable contributions include the search for binary in-spirals, hierarchical
methods, coherent search with a network of detectors and the radiometric
search for stochastic gravitational waves.
• IUCAA has collaborated with most international GW detector groups and has
been a member of the LIGO Scientific Collaboration.
• At IUCAA, Tarun Souradeep with expertise in CMB data and Planck has
worked to create a bridge between CMB and GW data analysis challenges.
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 multidetector detection, hierarchical techniques, noise characterisation 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 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 committee of IndIGO
High precision and Large experiment in India
•
C.S. Unnikrishnan (TIFR) : involved in high precision experiments and tests
–
–
–
•
Groups at BARC and RRCAT : involved in LHC
–
•
•
•
•
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)
–
–
•
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) :
–
–
–
•
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)
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.
2.
3.
4.
5.
6.
7.
8.
9.
CMI, Chennai
Delhi University
IISER Kolkata
IISER Trivandrum
IIT Madras (EE)
IIT Kanpur (EE)
IUCAA
RRCAT
TIFR
•
•
•
•
RRI
IPR, Bhatt
Jamia Milia Islamia
Tezpur Univ
The IndIGO Consortium
IndIGO Council
1.
2.
3.
4.
Bala Iyer
Sanjeev Dhurandhar
C. S. Unnikrishnan
Tarun Souradeep
( Chair)
(Science)
(Experiment)
(Spokesperson)
Data Analysis & Theory
Instrumentation & Experiment
1.
2.
3.
4.
5.
6.
7.
8.
9.
10.
11.
12.
13.
14.
15.
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
Rijuparna Chakraborty, Cote d’Azur, Grasse
Rana Adhikari
Caltech, USA
Suresh Doravari
Caltech, USA
Biplab Bhawal
(ex LIGO)
RRI, Bangalore
IUCAA, Pune
TIFR, Mumbai
IUCAA, Pune
1.
2.
3.
4.
5.
6.
7.
8.
9.
10.
11.
12.
13.
14.
15.
16.
17.
18.
19.
Sanjeev Dhurandhar
Bala Iyer
Tarun Souradeep
Anand Sengupta
Archana Pai
Sanjit Mitra
K G Arun
Rajesh Nayak
A. Gopakumar
T R Seshadri
Patrick Dasgupta
Sanjay Jhingan
L. Sriramkumar,
Bhim P. Sarma
P Ajith
Sukanta Bose,
B. S. Sathyaprakash
Soumya Mohanty
Badri Krishnan
IUCAA
RRI
IUCAA
Delhi University
IISER, Thiruvananthapuram
JPL , IUCAA
Chennai Math. Inst., Chennai
IISER, Kolkata
TIFR, Mumbai
Delhi University
Delhi University
Jamila Milia Islamia, Delhi
Phys., IIT M
Tezpur Univ .
Caltech , USA
Wash. U., USA
Cardiff University, UK
UTB, Brownsville , USA
Max Planck AEI, Germany
23 July 2011
Dear 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……
IndIGO Advisory Structure
Committees:
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)
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
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
IndIGO 3m Prototype Detector
Funded by TIFR Mumbai on compus (2010)
PI: C. S. Unnikrishnan (Cost ~ INR 2.5 crore)
V ibration isolation
s chem atic
Las er table
S e n s in g &
C o n tro l
180 cm
A ll m irros and beam splitters
are s uspended as in the diagram on right
P o w e r re c yc lin g
D etector
Vacuum
ta n k s
F -P c a v ity
0 .8 m
M irror
3.2 m eters
60 cm
IndIGO Data Centre@IUCAA
 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
Indo-US centre for Gravitational
Physics and Astronomy
APPROVED for funding (Dec 2010)
• Centre of the 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, IUCAA
US:
Caltech, WSU
- PI: Rana Adhikari, Caltech
LIGO-India from LIGO
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: 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: Why is it a good idea? …for India
• Have 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!
–
LIGO/ACIGA/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, 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, path defining,
International Experiment in India .”
LIGO-India: Salient points of this megaproject
• On Indian Soil will draw and retain science & tech. manpower
• International Cooperation, not competition LIGO-India success critical to the success
of the global GW science effort. Complete Intl support
• Shared science risk with International community 
Shared historical, major science discovery credit !!!
• AdvLIGO setup & initial challenge/risks primarily rests with USA.
– AdvLIGO-USA precedes LIGO-India by > 2 years.
– India sign up for technically demonstrated/established part (>10 yr of operation in initial LIGO ) 
2/3 vacuum enclosure + 1/3 detector assembly split (US ‘costing’ : manpower and h/ware costs)
– However, allows Indian scientist to collaborate on highly interesting science & technical challenges
of Advanced LIGO-USA ( ***opportunity without primary responsibility***)
• Expenditure almost completely in Indian labs & Industry huge potential for
landmark technical upgrade in all related Indian Industry
• Well defined training plan
core Indian technical team thru Indian postdoc in related exptal areas
participation in advLIGO-USA installation and commissioning phase, cascade to training at Indian expt. centers
• Major data analysis centre for the entire LIGO network with huge potential
for widespread University sector engagement.
• US hardware contribution funded & ready advLIGO largest NSF project, LIGOIndia needs NSF approval but not additional funds
LIGO-India: … the opportunity
Strategic Geographical relocation: science gain
Source localization error
Original plan
2 +1 LIGO USA+ Virgo
LIGO-India plan
1+1 LIGO USA+ Virgo+ LIGO India
LIGO-Aus plan
1+1 LIGO USA+ Virgo+ LIGO Aus
LIGO-India: … the opportunity
Strategic Geographical relocation: science gain
Polarization info
Homogeneity of Sky coverage
Courtesy: B. Schutz
LIGO-India: … the opportunity
Strategic Geographical relocation: science gain
Sky coverage
: Synthesized
Network
beam
(antenna power)
Courtesy: B. Schutz
LIGO-India: … the opportunity
Strategic Geographical relocation: science gain
Sky coverage: ‘reach’ /sensitivity in different directions
Courtesy: B. Schutz
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 modecleaner (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
LIGO-India vs. Indian-IGO ?
Primary advantage: LIGO-India Provides cutting edge instrumentation &
technology to jump start GW detection and astronomy.
Would require at least a decade of focused & sustained technology developments
in Indian laboratories and industry
•
180 W Nd:YAG: 5 years;
– 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
• Seismic isolation (BCE,HAM) .. Minimum 2 of years of expt and R&D.
– Experience in setting up and maintaining these systems  know how for
isolation in critical experiments such as in optical metrology,
AFM/Microscopy, gravity experiments etc.
• 10 interferometer core optics.. manufacturing optics of this quality and
develop required metrology facility : At least 5 to 7 years of
dedicated R&D work in optical polishing, figuring and metrology.
• Five quadruple stage large optics suspensions systems.. 3-4 years of
development.. Not trivial to implement.
– Benefit other physics experiments working at the quantum limit of noise.
LIGO-India: Expected Indian Contribution
• Indian contribution in infrastructure:
 Site (L-configuration: Each 50-100 m x 4.2 km)
 Vacuum system
 Related Controls
 Data centre
• Indian contribution in human resources:
 Trained manpower for installation and commissioning
 Trained manpower for LIGO-India operations for 10 years
 Simulation and Data Analysis teams
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 !!!!!
Technology Payoffs
• Lasers and optics..Purest laser light..Low phase noise, excellent
beam quality, high single frequency power
• Applications in precision metrology, medicine, micro-machining
• Coherent laser radar and strain sensors for earthquake prediction
and other precision metrology
• Surface accuracy of mirrors 100 times better than telescope
mirrors..Ultra-high reflective coatings : New technology for other fields
• Vibration Isolation and suspension..Applications for mineral prospecting
• Squeezing and challenging “quantum limits” in measurements.
• Ultra-high vacuum system 10^-9 tor (1picomHg). Beyond best in the
region
• Computation Challenges: Cloud computing, Grid computing, new
hardware and software tools for computational innovation.
Rewards and spinoffs
Detection of GW is the epitome of breakthrough science!!!
• LIGO-India  India could become a partner in international
science of Nobel Prize significance
• GW detection is an instrument technology intensive field pushing
frontiers simultaneously in a number of fields like lasers and
photonics. Impact allied areas and smart industries.
• The imperative need to work closely with industry and other end
users will lead to spinoffs as GW scientists further develop optical
sensor technology.
• Presence of LIGO-India will lead to pushing technologies and greater
innovation in the future.
• The largest UHV system will provide industry a challenge and
experience.
… rewards and spinoffs
• LIGO-India will raise public/citizen profile of science since it
will be making ongoing discoveries fascinating the young.
GR, BH, EU and Einstein have a special attraction and a pioneering facility in India
participating in important discoveries will provide science & technology role
models with high visibility and media interest.
• LIGO has a strong outreach tradition and LIGO-India will
provide a platform to increase it and synergetically benefit.
• Increase number of research groups performing at world
class levels and produce skilled researchers.
• Increase international collaborations in Indian research &
establishing 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 leader
Construction: Substantial Engg project building Indian capability in large
vacuum system engg, welding techniques and technology
 Complex Project must be well-coordinated and effectively carried out
in time and meeting the almost zero-tolerance specs
Train manpower for installation & commissioning
 Generate & sustain manpower running for 10 years.
 Site
 short lead time
 International competition (LIGO-Argentina ??)
Technical
 vacuum system
 Related Controls
 Data centre
LIGO-India: … the challenges
Trained Manpower for installation & commissioning
LIGO-India Director
Project manager
Project engineering staff:
Civil engineer(s)
Vacuum engineer(s)
Systems engineer(s),
Mechanical engineers
Electronics engineers
Software engineers
Detector leader
Project system engineer
Detector subsystem leaders
10 talented scientists or research engineers
with interest and knowledge collectively spanning:
Lasers and optical devices, Optical metrology, handling and cleaning,
Precision mechanical structures, Low noise electronics, Digital control systems
and electro-mechanical servo design, Vacuum cleaning and handling)
Logistics and Preliminary Plan
• Assumption: Project taken up by DAE as a National Mega
Flagship Project.
All the persons mentioned who are currently working in their centers would be mainly in a
supervisory role of working on the project during the installation phase and training manpower
recruited under the project who would then transition into the operating staff.
• Instrument Engineering: No manpower required for design and
development activity. For installation and commissioning phase
and subsequent operation
• Laser ITF: Unnikrishnan, Sendhil Raja, Anil Prabhaker.
TIFR, RRCAT, IITM. 10 Post-doc/Ph.D students. Over 2-3 years.
Spend a year at Advanced LIGO. 6 full time engineers and
scientists. If project sanctioned, manpower sanctioned, LIGOIndia project hiring at RRCAT, TIFR, other insitututions/Labs.
Large scale ultra-high Vacuum enclosure
S.K. Shukla (RRCAT),A.S. Raja Rao (ex RRCAT),
S. Bhatt (IPR), Ajai Kumar (IPR)
•To be fabricated by IndIGO with designs from LIGO. A pumped volume of
10000m3 (10Mega-litres), evacuated to an ultra high vacuum of 10-9 torr
(pico-m Hg).
o Spiral welded beam tubes 1.2m in diameter and 20m length.
o Butt welding of 20m tubes together to 200m length.
o Butt welding of expansion bellows between 200m tubes.
o Gate valves of 1m aperture at the 4km tube ends and the middle.
o Optics tanks, to house the end mirrors and beam splitter/power and signal
recycling optics vacuum pumps.
o Gate valves and peripheral vacuum components.
o Baking and leak checking
Large scale ultra-high Vacuum enclosure
• 5 Engineers and 5 technicians
o Oversee the procurement & fabrication of the vacuum system
components and its installation.
o If the project is taken up by DAE then participation of RRCAT & IPR is more
intense
o 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 support from RRCAT, IPR and LIGO Lab.
• Preliminary detailed discussions in Feb 2011 : companies like HHV,
Fullinger in consultation with Stan Whitcomb (LIGO), D. Blair (ACIGA) since this
was a major IndIGO deliverable to LIGO-Australia.
• Preliminary Costing for LIGO-India (vacuum component 400 cr)
Ultra-high Vacuum enclosure pictures
Logistics and Preliminary Plans
42 persons (10 PhD/postdocs, 22 scientists/engineers and 10 technicians)
• Mobile 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 & installation.
• Vibration isolation system: 2 engineers (precision mechanical)
– install and maintain the system. Sourced from BARC. RED (Reactor Engineering
Division of BARC) has a group that works on vibration measurement, analysis and
control in reactors and turbo machinery.
• Electronic Control System: 4 Engineers
– install and maintain the electronics control and data acquisition system.
Electronics & Instrumentation Group at BARC (G. P. Shrivastava’s group) and
RRCAT.
– Preliminary training:six months at LIGO. Primary responsibility (installing and
running the electronics control and data acquisition system): RRCAT & BARC.
Additional activity for LIGO-India can be factored in XII plan if the approvals
come in early.
… Logistics and Preliminary Plans
Teams at Electronics & Instrumentation Groups at BARC may be interested
in large instrumentation projects in XII plan.
• Control software Interface: 2 Engineers
– install and maintain the computer software interface, distributed
networking and control system). RRCAT and BARC. Computer software
interface (part of the data acquisition system) and is the “Humanmachine-interface” for the interferometer. For seamless
implementation man power to be sourced from teams implementing
Electronic Control System.
• Site Selection & Civil Construction
– BARC Seismology Division Data reg. seismic noise at various DAE sites
to do initial selection of sites and shortlist based on other
considerations such as accessibility and remoteness from road traffic
etc. DAE: Directorate of Construction, services and Estate Management
(DCSEM): Co-ordinate design and construction of the required civil
structures required for the ITF. 2 engineers + 3 technicians (design &
supervision of constructions at site). Construction contracted to
private construction firm under supervision of DCSEM.
LIGO-India: … the challenges
Manpower generation for sustenance of the LIGO-India observatory :
Preliminary Plans & exploration
• Since Advanced LIGO will have a lead time, participants will be identified
who will be deputed to take part in the commissioning of Advanced LIGO and
later bring in the experience to LIGO-India
• Successful IndIGO Summer internships in International labs
underway
o High UG applications 30/40 each year from IIT, IISER, NISERS,..
o 2 summers, 10 students, 1 starting PhD at LIGO-MIT
o Plan to extend to participating National labs to generate more experimenters
• IndIGO schools are planned annually to expose students to emerging
opportunity in GW science
o 1st IndIGO school in Dec 2010 in Delhi Univ. (thru IUCAA)
• Post graduate school specialization courses , or more
Jayant Narlikar: “Since sophisticated technology is involved IndIGO should like
ISRO or BARC training school set up a program where after successful
completion of the training, jobs are assured.”
Indian Site
LIGO-India: … the challenges
Requirements:
• Low seismicity
• Low human generated noise
• Air connectivity,
• Proximity to Academic institution, labs, industry
Preliminary exploration:
IISc new campus & adjoining campuses near Chitra Durga
• low seismicity
• 1hr from Intl airport
• Bangalore: science & tech hub
• National science facilities complex plans
•
•
LIGO-India: Action points
If 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 on LIGO India
• Home ground advantage !!! Once in a generation opportunity
• Threshold of discovery and launch of a new observational window
in human history!! Century after Einstein GR, 40 yrs of Herculean global effort
• Cooperative, not competitive science
• India at the forefront of GW science with 2nd generation of detectors:
Intl. shared science risks and credit
• Low project risk: commit to established tech. yet are able to take on
challenges of advLIGO (opportunity without primary responsibility)
“Every high
singletechnology
technology gains
they’refor
touching
pushing, and there’s
• Attain
Indian they’re
labs & industries
Thank you !!!
a lot of different technologies they’re touching.”
(Beverly Berger, National Science Foundation Program director for gravitational physics. )
• India pays true tribute to fulfilling Chandrasekhar’s legacy:
”Astronomy is the natural home of general relativity”
An unique once-in-a-generation opportunity for India. India could
play a key role in Intl. Science by hosting LIGO-India.
Deserves a National mega-science initiative
END
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 LIGOLab 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.
Thank you !!!
Detecting GW with Laser Interferometer
B
A
Path A
Path B
Difference in distance of Path A & B  Interference of laser
light at the detector (Photodiode)
Interferometry
Path difference of light  phase difference
Equal arms:
Dark fringe
The effects of gravitational
waves appear as a
fluctuation in the phase
differences between two
orthogonal light paths of an
interferometer.
Unequal arm:
Signal in PD
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
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
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
47.30%
79.00%
53.50%
0.66
2.02
3.01
Volume Filling
factor
Sky Coverage:
81%
Directional
Precision