LIGO-India Detecting Einstein

1
LIGO-IndiaDetecting Einsteins Elusive
WavesOpening a New Window to the Universe

• An Indo-US joint mega-project concept proposal

IndIGO Consortium (Indian
Initiative in Gravitational-wave Observations)
Version 1R Jun 17, 2011 TS
www.gw-indigo.org
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Space Time as a fabric
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.
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Space Time as a fabric
Earth follows a straight path in the curved
space-time caused by suns mass !!!
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Beauty Precision
Einsteins 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,.
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What happens when matter is in motion?
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• Einsteins 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 Newtons gravity
• Begs direct verification !!!

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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.

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GW ?? Astronomy link

• Astrophysical systems are sources of copious GW
  emission
• Typically, GW emission (0.1) gtgt EM radiation
  via Nuclear process (0.025)
• Energy emitted in GW from binary gtgt 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

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GW from Binary Neutron stars
Pulsar
companion
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Indirect evidence for Gravity waves
Nobel prize in 1993 !!!
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

Hulse and Taylor Results for PSR191316
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Principle behind Detection of GW
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Effect of GW on a ring of test masses
Interferometer mirrors as test masses
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Detecting GW with Laser Interferometer
B
A
Difference in distance of Path A B ?
Interference of laser light at the detector
(Photodiode)
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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
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Challenge of Direct Detection
Gravitational wave is measured in terms of
strain, h (change in length/original length)
Gravitational waves are very weak!
Expected amplitude of GW signals
Measure changes of one part in
thousand-billion-billion!
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LIGO Optical Configuration
Michelson Interferometer
input test mass
Laser
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Initial LIGO Sensitivity Goal

• Strain sensitivity lt3x10-23 1/Hz1/2at 200 Hz

• Sensor Noise
• Photon Shot Noise
• Residual Gas
• Displacement Noise
• Seismic motion
• Thermal Noise
• Radiation Pressure

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LIGO and Virgo TODAY
Milestone Decades-old plans to build and
operate large interferometric GW detectors now
realized at several locations worldwide Experiment
al 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..

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Laser Interferometer Gravitational-wave
Observatory (LIGO)
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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

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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

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Advanced LIGO

• Take advantage of new technologies and on-going
  RD
• gtgt Active anti-seismic system operating to lower
  frequencies
• (Hannover, GEO)
• gtgt Lower thermal noise suspensions and optics
• (GEO )
• gtgt Higher laser power 10 W ? 180 W
• (Hannover group, Germany)
• gtgt 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

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• 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 !!!

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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

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Schematic Optical Design of Advanced LIGO
detectors
Reflects International cooperation Basic nature
of GW Astronomy
LASER AEI, Hannover Germany
Seismic isolation Suspension GEO, UK
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Advanced LIGO Laser

• Designed and contributed by Albert Einstein
  Institutelt Germany
• Higher power
• 10W -gt 180W
• Better stability
• 10x improvement in intensity and frequency
  stability

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Advanced LIGO Mirrors

• Larger size
• 11 kg -gt 40 kg
• Smaller figure error
• 0.7 nm -gt 0.35 nm
• Lower absorption
• 2 ppm -gt 0.5 ppm
• Lower coating thermal noise

• All substrates delivered
• Polishing underway
• Reflective Coating process starting up

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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 -gt 10 Hz

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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 -gt 108
• Suppression at 10 Hz ?
• at 1 Hz ?

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Era of Advanced LIGO detectors 2015

• 10x sensitivity
• 10x reach
• 1000 volume
• gtgt 1000 event rate
• (reach beyond
• nearest super-clusters)
• A Day of Advanced LIGO Observation gtgt
• A year of Initial LIGO

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Expected Annual Coalescence Event Rates
Detector 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 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.
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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

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GW Astronomy with Intl. Network of GW
Observatories
1. Detection confidence 2. Duty cycle 3.
Source direction 4. Polarization info.
LIGO-India ?
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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..

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vit
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

GWIC Roadmap Document
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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.

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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

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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.

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• 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

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The IndIGO Consortium

• IndIGO Council
• Bala Iyer ( Chair) RRI,
  Bangalore
• Sanjeev Dhurandhar (Science) IUCAA, Pune
• C. S. Unnikrishnan (Experiment) TIFR, Mumbai
• Tarun Souradeep (Spokesperson) IUCAA, Pune

• Data Analysis Theory
• Sanjeev Dhurandhar IUCAA
• Bala Iyer RRI
• Tarun Souradeep IUCAA
• Anand Sengupta Delhi University
• Archana Pai IISER,
  Thiruvananthapuram
• Sanjit Mitra JPL , IUCAA
• K G Arun Chennai Math. Inst., Chennai
• Rajesh Nayak IISER, Kolkata
• A. Gopakumar TIFR, Mumbai
• T R Seshadri Delhi University
• Patrick Dasgupta Delhi University
• Sanjay Jhingan Jamila Milia Islamia, Delhi
• L. Sriramkumar, Phys., IIT M
• Bhim P. Sarma Tezpur Univ .
• P Ajith Caltech , USA
• Sukanta Bose, Wash. U., USA
• B. S. Sathyaprakash Cardiff University, UK

• Instrumentation Experiment
• C. S. Unnikrishnan TIFR, Mumbai
• G Rajalakshmi TIFR, Mumbai
• P.K. Gupta RRCAT, Indore
• Sendhil Raja RRCAT, Indore
• S.K. Shukla RRCAT, Indore
• Raja Rao ex RRCAT, Consultant
• Anil Prabhakar, EE, IIT M
• Pradeep Kumar, EE, IIT K
• Ajai Kumar IPR, Bhatt
• S.K. Bhatt IPR, Bhatt
• Ranjan Gupta IUCAA, Pune
• Rijuparna Chakraborty, Cote dAzur, Grasse
• Rana Adhikari Caltech, USA
• Suresh Doravari Caltech, USA
• Biplab Bhawal (ex LIGO)

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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
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IndIGO Advisory Structure
Committees
National Steering Committee Kailash Rustagi
(IIT, Mumbai) ChairBala Iyer (RRI)
CoordinatorSanjeev Dhurandhar (IUCAA)
Co-CoordinatorD.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 ChairKazuaki 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)
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)
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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.

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IndIGO 3m Prototype Detector
Funded by TIFR Mumbai on compus (2010) PI C.
S. Unnikrishnan (Cost INR 2.5 crore)
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IndIGO Data Centre_at_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
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Indo-US centre for Gravitational Physics and
Astronomy
APPROVED for funding (Dec 2010)

• 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

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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 from LIGO
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 RD effort
that preceded the success of Initial LIGO
gravitational wave detectors and the design of
their advanced version.
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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.

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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.

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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 gt 2 years.
• India sign up for technically demonstrated/establ
  ished part (gt10 yr of operation in initial LIGO )
  ? 2/3 vacuum enclosure 1/3 detector assembly
  split (US costing manpower and h/ware costs)
• However, allows Indian scientist to collaborate
  on highly interesting science technical
  challenges of Advanced LIGO-USA ( opportunity
  without primary responsibility)
• Expenditure almost completely in Indian labs
  Industry huge potential for landmark technical
  upgrade in all related Indian Industry
• Well defined training plan core Indian technical
  team thru Indian postdoc in related exptal areas
  participation in advLIGO-USA installation and
  commissioning phase, cascade to training at
  Indian expt. centers
• Major data analysis centre for the entire LIGO
  network with huge potential for widespread
  University sector engagement.
• US hardware contribution funded ready advLIGO
  largest NSF project, LIGO-India needs NSF
  approval but not additional funds

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LIGO-India the opportunity
Strategic Geographical relocation science gain
Source localization error
Original plan 2 1 LIGO USA Virgo
LIGO-India plan 11 LIGO USA Virgo LIGO India
LIGO-Aus plan 11 LIGO USA Virgo LIGO Aus
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LIGO-India the opportunity
Strategic Geographical relocation science gain
Polarization info
Homogeneity of Sky coverage
Courtesy B. Schutz
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LIGO-India the opportunity
Strategic Geographical relocation science gain
Sky coverage Synthesized Network
beam (antenna power)
Courtesy B. Schutz
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LIGO-India the opportunity
Strategic Geographical relocation science gain
Sky coverage reach /sensitivity in different
directions
Courtesy B. Schutz
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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
57
LIGO-India unique once-in-a-generation
opportunity
LIGO labs ?LIGO-India

• 180 W pre-stabilized NdYAG laser
• 10 interferometer core optics (test masses,
  folding mirrors, beam splitter, recycling
  mirrors)
• Input condition optics, including electro-optic
  modulators, Faraday isolators, a suspended
  mode-cleaner (12-m long mode-defining cavity),
  and suspended mode-matching telescope optics.
• 5 "BSC chamber" seismic isolation systems (two
  stage, six degree of freedom, active isolation
  stages capable of 200 kg payloads)
• 6 "HAM Chamber" seismic isolation systems (one
  stage, six degree of freedom, active isolation
  stages capable of 200 kg payloads)
• 11 Hydraulic External Pre-Isolation systems
• Five quadruple stage large optics suspensions
  systems
• Triple stage suspensions for remaining suspended
  optics
• Baffles and beam dumps for controlling
  scattering and stray radiation
• Optical distortion monitors and thermal
  control/compensation system for large optics
• Photo-detectors, conditioning electronics,
  actuation electronics and conditioning
• Data conditioning and acquisition system,
  software for data acquisition
• Supervisory control and monitoring system,
  software for all control systems
• Installation tooling and fixturing

58
LIGO-India vs. Indian-IGO ?

• Primary advantage LIGO-India Provides cutting
  edge instrumentation technology to jump start
  GW detection and astronomy.
• Would require at least a decade of focused
  sustained technology developments in Indian
  laboratories and industry
• 180 W Nd-Yag 5 years Rs. 10-12 crores.
• Operation and maintenance should benefit further
  development in narrow line width lasers.
• Applications in high resolution spectroscopy,
• precision interferometry and metrology.
• Input condition optics..Expensive..No Indian
  manufacturer with such specs
• BSC, HAM.. Minimum 2 of years of experimentation
  and RD.
• Experience in setting up and maintaining these
  systems ? know how forisolation in critical
  experiments such as in optical metrology,AFM/Micr
  oscopy, gravity experiments etc.
• 10 interferometer core optics.. manufacturing
  optics of this quality and develop required
  metrology facility At least 5 to 7 years
  ofdedicated RD work in optical polishing,
  figuring and metrology.
• Five quadruple stage large optics suspensions
  systems.. 3-4 years of development.. Not trivial
  to implement.
• Benefit other physics experiments working at the
  quantum limit of noise.

59

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

60
The Science Payoffs

• New Astronomy, New Astrophysics, New Cosmology,
  New Physics
• A New Window ushers a New Era of Exploration in
  Physics Astronomy
• Testing Einsteins 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, LMXBs, Magnetars
• New cosmology..SMBHBs as standard sirens..EOS of
  Dark Energy
• Phase transition related to fundamental
  unification of forces
• Multi-messenger astronomy
• The Unexpected !!!!!

61
The Technology Payoffs

• Lasers and optics..Purest laser light..Low phase
  noise, excellent beam quality, high single
  frequency power
• Applications in precision metrology, medicine,
  micro-machining
• Coherent laser radar and strain sensors for
  earthquake prediction and other precision
  metrology
• Surface accuracy of mirrors 100 times better than
  telescope mirrors..Ultra-high reflective
  coatings New technology for other fields
• Vibration Isolation and suspension..Applications
  for mineral prospecting
• Squeezing and challenging quantum limits in
  measurements.
• Ultra-high vacuum system 10-9 tor (1picomHg).
  Beyond best in the region
• Computation Challenges Cloud computing, Grid
  computing, new hardware and software tools for
  computational innovation.

62
The rewards and spinoffs

• Detection of GW is the epitome of breakthrough
  science!!!
• LIGO-India ? India could become a partner in
  international science of Nobel Prize significance
• GW detection is an instrument technology
  intensive field pushing frontiers simultaneously
  in a number of fields like lasers and photonics.
  Impact allied areas and smart industries.
• The imperative need to work closely with industry
  and other end users will lead to spinoffs as GW
  scientists further develop optical sensor
  technology.
• Presence of LIGO-India will lead to pushing
  technologies and greater innovation in the
  future.
• The largest UHV system will provide industry a
  challenge and experience.

63
rewards and spinoffs

• LIGO-India will raise public/citizen profile of
  science since it will be making ongoing
  discoveries fascinating the young.
• GR, BH, EU and Einstein have a special attraction
  and a pioneering facility in India participating
  in important discoveries will provide science
  technology role models with high visibility and
  media interest.
• LIGO has a strong outreach tradition and
  LIGO-India will provide a platform to increase it
  and synergetically benefit.
• Increase number of research groups performing at
  world class levels and produce skilled
  researchers.
• Increase number of businesses investing in RD.
  Provide opportunities to increase proportion of
  industries engaging in innovation.
• Increase international collaborations in Indian
  research establishing Science Leadership in the
  Asia-Pacific region.

64

• LIGO-India the challenges
• Organizational
• National level DST-DAE Consortium Flagship
  Mega-project
• Identify a lead institution and agency
• Project leader
• Construction Substantial Engg project building
  Indian capability in large vacuum system engg,
  welding techniques and technology
• Complex Project must be well-coordinated and
  effectively carried out
• in time and meeting the almost
  zero-tolerance specs
• Train manpower for installation commissioning
• Generate sustain manpower running for 10
  years.
• Site
• short lead time
• International competition (LIGO-Argentina ??)
• Technical
• vacuum system
• Related Controls
• Data centre

65
LIGO-India the challenges
Trained Manpower for installation commissioning
LIGO-India Director Project manager Project
engineering staff Civil engineer(s) Vacuum
engineer(s) Systems engineer(s), Mechanical
engineers Electronics engineers Software
engineers Detector leader Project system
engineer Detector subsystem leaders 10
talented scientists or research engineers with
interest and knowledge collectively
spanning Lasers and optical devices, Optical
metrology, handling and cleaning, Precision
mechanical structures, Low noise electronics,
Digital control systems and electro-mechanical
servo design, Vacuum cleaning and handling)

66
Logistics and Preliminary Plan

• Assumption Project taken up by DAE as a
  National Mega Flagship Project.
• All the persons mentioned who are currently
  working in their centers would be mainly in a
  supervisory role of working on the project during
  the installation phase and training manpower
  recruited under the project who would then
  transition into the operating staff.
• Instrument Engineering No manpower required for
  design and development activity. For installation
  and commissioning phase and subsequent operation
• Laser ITF Unnikrishnan, Sendhil Raja, Anil
  Prabhaker.
• TIFR, RRCAT, IITM. 10 Post-doc/Ph.D students.
  Over 2-3 years.
• Spend a year at Advanced LIGO. 6 full time
  engineers and scientists. If project sanctioned,
  manpower sanctioned, LIGO-India project hiring at
  RRCAT, TIFR, other insitututions/Labs.
•  

67
Large scale ultra-high Vacuum enclosure S.K.
Shukla (RRCAT),A.S. Raja Rao (ex RRCAT), S.
Bhatt (IPR), Ajai Kumar (IPR)

• To be fabricated by IndIGO with designs from
  LIGO. A pumped volume of 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

68
Large scale ultra-high Vacuum enclosure

• 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 LT,
  Fillunger, HindHiVac, Godrej with support from
  RRCAT, IPR and LIGO Lab.
• Preliminary detailed discussions in Feb 2011
  with companies like HHV, Fullinger in
  consultation with Stan Whitcomb (LIGO), D. Blair
  (ACIGA) since this was a major IndIGO
  deliverable to LIGO-Australia
• Preliminary Costing for LIGO-India (vacuum 400
  cr)

69
Logistics and Preliminary Plans

• 42 persons (10 PhD/postdocs, 22
  scientists/engineers and 10 technicians)
• Clean rooms
• Movable tent type clean rooms during welding of
  the beam tubes and assembly of the system. Final
  building a clean room with AC and pressurization
  modules. SAC, ISRO. 1 engineer and 2 technicians
  to draw specs for the clean room equipments and
  installation.
• Vibration isolation system 2 engineers
  (precision mechanical)
• install and maintain the system. Sourced from
  BARC. RED (Reactor Engineering Division of BARC)
  has a group that works on vibration measurement,
  analysis and control in reactors and turbo
  machinery.
• Electronic Control System 4 Engineers
• install and maintain the electronics control and
  data acquisition system. Electronics
  Instrumentation Group at BARC (G. P.
  Shrivastavas group) and RRCAT.
• Preliminary trainingsix months at LIGO. Primary
  responsibility (installing and running the
  electronics control and data acquisition system)
  RRCAT BARC. Additional activity for LIGO-India
  can be factored in XII plan if the approvals
  come in early.

70
Logistics and Work Plan

• Teams at Electronics Instrumentation Groups at
  BARC may be interested in large instrumentation
  projects in XII plan.
• Control software Interface 2 Engineers
• install and maintain the computer software
  interface, distributed networking and control
  system). RRCAT and BARC. Computer software
  interface (part of the data acquisition system)
  and is the Human-machine-interface for the
  interferometer. For seamless implementation man
  power to be sourced from teams implementing
  Electronic Control System.
• Site Selection Civil Construction
• BARC Seismology Division Data reg. seismic noise
  at various DAE sites to do initial selection of
  sites and shortlist based on other considerations
  such as accessibility and remoteness from road
  traffic etc. DAE Directorate of Construction,
  services and Estate Management (DCSEM)
  Co-ordinate design and construction of the
  required civil structures required for the ITF.
  2 engineers 3 technicians (design supervision
  of constructions at site). Construction
  contracted to private construction firm under
  supervision of DCSEM.

71
LIGO-India the challenges
Manpower generation for sustenance of the
LIGO-India observatory Preliminary Plans
exploration

• Since Advanced LIGO will have a lead time,
  participants will be identified who will be
  deputed to take part in the commissioning of
  Advanced LIGO and later bring in the experience
  to LIGO-India
• Successful IndIGO Summer internships in
  International labs underway
• High UG applications 30/40 each year from IIT,
  IISER, NISERS,..
• 2 summers, 10 students, 1 starting PhD at
  LIGO-MIT
• 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
• 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.

72
LIGO-India the challenges
Indian Site
Requirements Low seismicity Low human generated
noise Air connectivity, Proximity to Academic
institution, labs, industry

• Preliminary exploration
• IISc new campus adjoining campuses near Chitra
  Durga
• 1hr from Intl airport
• low seismicity
• National science facilities complex plans

73
Concluding remarks

• A century after Einsteins 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 Indias
  share of task (other part opportunity w/o
  responsibility)
• National mega-science initiative Need strong
  multi-institutional support to bring together
  capable scientists technologist in India
• An unique once-in-a-generation opportunity for
  India. India could play a key role in Intl.
  Science by hosting LIGO-India.

74
Concluding remarks

• A GREAT opportunity but a very sharp deadline of
  31 Mar 2012. If we cannot act quickly the
  possibility will close. Conditions laid out in
  the Request Doc of LIGO-Lab will need to be ready
  for LIGO-Lab examination latest by Dec 2011 so
  that in turn LIGO-Lab can make a case with NSF by
  Jan 2012.
• Of all the large scientific projects out there,
  this one is pushing the greatest number of
  technologies the hardest.
• Every single technology theyre touching theyre
  pushing, and theres a lot of different
  technologies theyre touching.
• (Beverly Berger, National Science
  Foundation Program director for gravitational
  physics. )
• One is left speculating if by the centenary of
  General Relativity in 2015, the first discovery
  of Gravitational waves would be from a Binary
  Black Hole system, and Chandrasekhar would be
  doubly right about
• Astronomy being the natural home of general
  relativity.

75
LIGO-India Action points

• If accepted as a National Flagship Mega Project
  under the 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

Thank you !!!