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: BRI Jun 10, 2011
Space Time as a fabric
In 1916, Albert Einstein published his famous Theory of General
Relativity, the theory of gravitation.
4-dimensional space-time (the normal three dimensions of space, plus
a fourth dimension of time).
His theory describes how space-time is affected by mass
and also how mass affects spacetime.
Matter tells spacetime how to curve, and spacetime tells matter
how to move.
Space Time as a fabric
Einstein’s General theory of relativity
is the most
beautiful & successful
theory of modern physics.
It has matched all tests of
Gravitation remarkably well.
What happens when matter is in
motion?
Einstein’s theory predicts
Matter in motion fluctuation in the
curvature of space-time which
propogates as a wave
Space-time ripples or gravitational
waves
Binary Neutron stars
Pulsar
companion
GW from Binary Neutron stars
Indirect evidence for Gravity waves
Binary pulsar emits gravitational waves
1.
2.
3.
4.
leads to loss of orbital
energy
period speeds up 14 sec
from 1975-94
measured to ~50 msec
accuracy
deviation grows
quadratically with time
Won the Nobel prize
in 1993 !!!
Hulse and Taylor
Results for PSR1913+16
Effect of GW on test masses
Effect of GW on a ring of test masses
Interferometer mirrors as test masses
Detecting GW with Laser Interferometer
A
B
Path A
Path B
Difference in distance of Path A & B  Interference of laser light at the
detector (Photodiode)
Path difference  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
Challenge of Direct Detection
Gravitational waves are very weak!
Gravitational wave is measured in
terms of strain,
h
(change in length/original length)
Expected amplitude of GW
signals
Measure changes of
2
L
L
h  10
20
h
 10
23
one part in thousand-billion-billion!
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
TAMA: 0.3km
LCGT
LIGO-LLO: 4km
LIGO-Australia?
LIGO-India ?
A Century of Waiting
•Almost 100 years since GW were theoretically predicted By Albert
Einstein but still no direct experimental confirmation a la Hertz
•Reason is connected to two fundamental differences between EM and
Gravitation:
- The weakness of the gravitational interaction relative to EM (10􀀀39)
-The spin two nature of gravitation compared to the spin one nature
of EM that forbids dipole radiation in GR.
•Implies low efficiency for conversion of mechanical energy to gravitational
radiation. And feeble effects of GW on any potential detector.
•A GW Hertz experiment is ruled out and it is only signals produced by
astrophysical systems where there are potentially huge masses
accelerating very strongly that are likely sources.
Gravitational Waves Exist!
High quality data which is proof that GW exist.
In 1974 Hulse and Taylor, discovered the Binary Pulsar 1913+16.
The system has now been monitored for 30 years. Orbital period slowly
decreasing at just the rate predicted by GR for emission of GW!!!
Hulse and Taylor received Nobel Prize for this (1993).
ADD FIGURES
Laser Interferometric Gravitational Wave Detectors?
•Binary Pulsars establish Reality of Grav Radn. Validity of GR in Strong Fields.
Excellent Evidence but Evidence is Indirect
•Can detectors be built to attempt a Direct detection of these GW??
•GW are transverse and tidally distort a system in directions
perpendicular to propagation direction.
•Effect measured by the Dimensionless strain h = 2( Delta L)/ L, it produces
For a typical NS binary in Virgo cluster (18 Mpc; 5.6 x 10^20 km)
h = 4G/ c^4 Knonsph/D ~ (2 GM/ Rc^2) (GM/Dc^2) ~ 1.5 x 10^-21
•The miniscule strain and associated tiny displacement must be
measured to detect the GW.
•Weber's Bar detectors (Narrow band);
Today's Laser Interferometric Detectors ( Broad Band)
•As a GW passes, the arm lengths of km scale ITF change (10^-18m)
tidally causing the interference pattern to change at the photodiode
•Direct detection of GW First mandate of Laser Interferometric GW detectors
•Promised and Real Excitement - New Observational Window and
Tool for Astrophysics; Experimental Probe for Basic Physics
Change in Length manifests as Change in Transmitted Light
GW detection is about seeing the biggest things that ever happen by measuring
the smallest changes that have ever been measured - Harry Collins.
LIGO
and
Virgo
TODAY
Field reached a Milestone with decades-old plans to build and operate large
interferometric GW detectors now realized at several locations worldwide
Unprecedented sensitivity allows one to place Upper Limits on GW from a
variety of Ap sources. Improve on Spindown of Crab, Vela pulsars,
Big Bang nucleosynthesis bound on Stochastic GW..
Expected Annual Coalescence Rates
In a 95% condence 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.
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
Laser Interferometer GW Observatory
40 kg
Fused silica
mirrors
(USA)
Optics & controls
(USA)
180 W
(Germany)
Fig from LIGO-AUS report?
Schematic Optical Design of Advanced LIGO detectors
Era of Advanced LIGO detectors: 2015
If retained get better res picture
Gravitational wave Astronomy :
Synergy with other major Astronomy projects:
• SKA: Radio : Pulsars timing,
• X-ray satellite (AstroSAT)
• Gamma ray observatory
•Thirty meter telescope: gamma ray follow-up,…
•
•
Courtesy: B. Schutz, GWIC Roadmap Document 2010
INDIGO: the goals
•
Major experimental science science initiative in GW astronomy
 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 armlength high vacuum tubes in L config.
– Indian cost ~Rs 1000Cr
 Earlier plan: Partnership 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.
• Consolidated IndIGO membership of LIGO Scientific Collaboration
+ propose creating a Tier-2 data centre for LSC in IUCAA + IUSSTF IndoUS joint
Centre at IUCAA with Caltech (funded)
• 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 | High Vaccum & controls at RRCAT, IPR, BARC,
ISRO, ….
– UG summer internship at Natn. & Intl GW labs & observatories.
– Postgrad IndIGO schools, specialized courses,…
Multi-Institutional,
Multi-disciplinary Consortium
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9.
CMI, Chennai
Delhi University
IISER Kolkata
IISER Trivandrum
IIT Madras
IIT Kanpur
IUCAA
RRCAT
TIFR
•
•
•
•
RRI
IPR, Bhatt
Jamia Milia Islamia
Tezpur Univ
The IndIGO Consortium
IndIGO Council
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2.
3.
4.
Bala Iyer
Sanjeev Dhurandhar
C. S. Unnikrishnan
Tarun Souradeep
( Chair)
(Science)
(Experiment)
(Spokesperson)
Data Analysis & Theory
Instrumentation & Experiment
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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
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3.
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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
IndIGO Advisory Structure
Committees:
International Advisory Committee
Abhay Ashtekar (Penn SU)[ Chair]
Rana Adhikari (LIGO, Caltech, USA)
David Blair (AIGO, UWA, Australia)
Adalberto Giazotto (Virgo, Italy)
P.D. Gupta (Director, RRCAT, India)
James Hough (GEO ; Glasgow, UK)[GWIC Chair]
Kazuaki Kuroda (LCGT, Japan)
Harald Lueck (GEO, Germany)
Nary Man (Virgo, France)
Jay Marx (LIGO, Director, USA)
David McClelland (AIGO, ANU, Australia)
Jesper Munch (Chair, ACIGA, Australia)
B.S. Sathyaprakash (GEO, Cardiff Univ, UK)
Bernard F. Schutz (GEO, Director AEI, Germany)
Jean-Yves Vinet (Virgo, France)
Stan Whitcomb (LIGO, Caltech, USA)
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)
INSERT
LIGO-India: Why is it a good idea?
for India
• Has a 20 year legacy and wide recognition in the Intl. GW community with
seminal contributions to Source modeling (RRI)& Data Analysis (IUCAA). High
precision measurements (TIFR), Participation in LHC (RRCAT)
•
(Would not make it to the GWIC report, otherwise!)
–
AIGO/LIGO/EGO strong interest in fostering Indian community
– GWIC invitation to IndIGO join as member (July 2011)
• Provides an exciting challenge at an International forefront of experimental
science. Can tap and siphon back the extremely good UG students trained in
India. (Sole cause of `brain drain’).
– 1st yr summer intern 2010  MIT for PhD
– Indian experimental scientist  Postdoc at LIGO training for Adv. LIGO subsystem
• Indian experimental expertise related to GW observatories will thrive and attain
high levels due to LIGO-India.
– Sendhil Raja, RRCAT, Anil Prabhakar, EE, IIT Madras, Pradeep Kumar, EE, IITK Photonics
– Vacuum expertise with RRCAT (S.K. Shukla, A.S. Raja Rao) , IPR (S.K. Bhatt, Ajai Kumar)
• Jump start direct participation in GW observations/astronomy
–
going beyond analysis methodology & theoretical prediction --- to full fledged
participation in experiment, data acquisition, analysis and astronomy results.
• For once, may be perfect time to a launch into a promising field (GW
astronomy) with high end technological spinoffs well before it has obviously
blossomed. Once in a generation opportunity to host an Unique
International Experiment here.
LIGO-India: Why is it a good idea?
… for the World
• Strategic geographical relocation for GW astronomy
– sky coverage gain
– distance:
– duty cycle:
• 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.
GWIC: Gravitational Wave International Committee
Courtesy: B. Schutz: GWIC Roadmap Document
Indo-Aus.Meeting, Delhi, Feb
2011
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……
LIGO-India: the concept …
• LIGO Lab approached with concept proposal for
joint mega-project --- strategic geographical
relocation of
• Advanced LIGO interferometer detector funded and
ready to be shipped by US
• Indian contribution in infrastructure :
 site
 vacuum system
Related Controls
Data centre
 trained manpower for installation,
commissioning and running for 10 years
The Science payoffs
•New Physics, New Astronomy, New Astrophysics, New Cosmology..
•A New Window ushers a new era of exploration..
•Testing Einstein's GR..
•Black hole phenomena..
•Understanding nuclear matter by neutron star EOS
•Neutron star coalescence events
•Listening to most energetic events in the universe.
Supernovae, Gamma ray bursts, Magnetars
•New Cosmology: Standard Sirens..Determine EOS of Dark energy
•Multi-messenger Astronomy
The Unexpected!!
The Technology Payoffs
f
•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.
Ultrahigh reflective coatings..
•Vibration isolation and suspension..Applications for mineral
prospecting
•Sqeezing and QM limits
•Ultra high vacuum system 10^-9 torr..
•Largest in this region
•Computation Challenges
LIGO-India: … the Opportunity
• Part of a fundamental scientific discovery : direct
detection of gravitational radiation
• Part of “historic” launch of a new window of Astronomy
•LIGO-India: Southernmost, hence, Unique role in the
Intl. GW observatory network.
• Full detector at about half the cost is the naïve
calculation.
Adv. LIGO detector system is worth 15 years of challenging R &D – price tag?
• Indian Labs & Industry
•
•
LIGO-India: … the opportunity
Strategic Geographical relocation
- the science gain
Sky coverage
: Synthesized
Network
beam
(antenna power)
LIGO-India: … the opportunity
Strategic Geographical relocation
- the science gain
Sky coverage: ‘reach’ /sensitivity in different directions
LIGO-India: … the opportunity
Strategic Geographical relocation
Source localization error
5-15 degrees to
~degree !!!
Ellipses version as in LIGO-Aus proposal ?
LIGO-India: … the opportunity
Strategic Geographical relocation
Polarization info
Sky coverage ?
LIGO-India: … the opportunity
Strategic Geographical relocation
Figure?
Network: HIJLV
Mean horizon distance:
Detection Volume:
Volume Filling factor:
Triple Detection Rate(80%):
Triple Detection Rate(95%):
Sky Coverage:
Directional Precision:
GMRT
1.57
12.0
73%
8.62
11.1
100%
2.93
Bangalore
1.63
12.0
66%
8.64
11.1
100%
3.00
LIGO-India: … the opportunity
LIGO-India : Technology gain
Relative valuation ?
• 180 W pre-stablized Nd:YAG laser
• Input condition optics, including electro-optic modulators, Faraday isolators, a
suspended mode-cleaner (12-m long mode-defining cavity), and suspended modematching telescope optics.
• five "BSC chamber" seismic isolation systems (two stage, six degree of freedom,
active isolation stages capable of ~200 kg payloads)
• six "HAM Chamber" seismic isolation systems (one stage, six degree of freedom,
active isolation stages capable of ~200 kg payloads)
• eleven Hydraulic External Pre-Isolation systems (mount external to chamber for
longer range and lower frequency isolation and actuation
• 10 interferometer core optics (test masses, folding mirrors, beam splitter, recycling
mirrors)
LIGO-India: … the opportunity
LIGO-India : Technology gain
Relative valuation ?
* 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
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: … the challenges
Organizational
 National level mega-project
 Identify a lead institution and agency
 Project leader
Train manpower for installation & commissioning
 Generate & sustain manpower running for 10 years.
 Site
 short lead time
 International competetion
Technical
 vacuum system
 Related Controls

 Data centre
LIGO-India: … the challenges
Trained Manpower for installation & commissioning
Requirements:
From LIGO requirements doc
Plans & Preliminary exploration:
Sendhil doc
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
LIGO-India: … the challenges
Generate manpower for sustenance of the Intl. observatory
Requirements:
Plans & Preliminary exploration:
• Summer internships in Intl labs underway
• IndIGO schools
Proposals:
Post graduate school specialization course
LIGO-India: … the challenges
Large scale ultra-high Vacuum enclosure
Requirements:
Preliminary exploration:
Indian Site
LIGO-India: … the challenges
Requirements:
Low seismicity
Low human generated noise
Air connectivity,
Acad institution, labs, industry
Preliminary exploration:
IISc new campus & adjoining campuses near Chitra Durga
•1hr from Intl airport
• low seismicity
•National science facilities complex plans
•
•
LIGO-India: … the challenges
Short lead time
Requirements:
Preliminary exploration:
LIGO-India: … the challenges
Internation competition
Issues:
Preliminary assessment:
LIGO-India
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!!
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.
The IndIGO data analysis centre
 Tier -2 centre with data archival and
computational facilities
•LIGO Sites at Hanford,
Livingston
•Data acquisition systems
 Inter-institutional proposal for facility
•LIGO Labs at Caltech
 Propose for a high-throughput
Computation and GW Data Archival
Centre.
•LIGO Lab at MIT, LSC institutions
like UWM, Syracuse etc
•IndIGO Data Analysis Centre
 Will provide fundamental infrastructure
for consolidating GW data analysis
expertise in India.
Courtesy: Anand Sengupta
Objectives of the data centre
Archival
Indian Researchers and
Students
TIER3 centres at
Univ & IISERS
LSC
LIGO Data Grid
Tier 2
Data Centre
at IUCAA
Community
development
Analysis
Other
science
groups
Web Services
Collaboration
tools
LIGO Data Grid as a role model for the proposed
IndIGO Data Analysis Centre.
Courtesy: Anand Sengupta
IndIGO Data Centre@IUCAA
Indian Initiative in Gravitational-wave Observations
 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
 100 Tflops = 8500 cores x 3 GHz/core
Need 8500 cores to carry out a half decent coherent search for gravitational
waves from compact binaries.
(1 Tflop = 250 GHz = 85 cores x 3 GHz / core)
 Storage: 4x100TB per year per interferometer.
 Network: gigabit backbone, National Knowledge Network.
Courtesy: Anand Sengupta, IndIGO
Future GWDA Plans of IndIGO
(as part of LSC)
Project leads: Sanjit Mitra, T. Souradeep, S. Dhurandhar …
 Extend GW radiometer work (Mitra,Dhurandhar, TS,…2009)
Implementation of the cross-correlation search for
periodic sources (Dhurandhar + collab.)
 Burst Sources
• Formulation
• Implementation
Courtesy: S. Dhurandhar
Vetoes for non-Gaussian noise for
coherent detection of inspirals
•
Project leads: Anand Sengupta, Archana Pai, M K Harris.
 Non-Gaussian noise plagues the detector data
 Vetoes have been developed in LSC for removal of non-Gaussian noise
in the single detector case
 For coincidence search the veto is obvious but for coherent not so.
 Developing a veto for coherent is crucial – chi squared
 Scope for improving the current chi squared test – Japanese
collaboration
Courtesy:
S. Dhurandhar
8th February
Delhi
Tests of General Relativity using GW
observations
Project leads: K G Arun, Rajesh Nayak and Chandra Kant Mishra,
Bala Iyer
 GWs are unique probes of strong field gravity. Their direct
detection would enable very precise tests of GR in the
dynamical and strong field regime.
 Preparing data analysis algorithms for AdvLIGO in order to
test GR and its alternatives is one of the important and
immediate goals of LSC.
 Plan to take part in the activity to develop parameter
estimation tools based on Bayesian methods.
 Possible collaboration with B S Sathyaprakash (Cardiff
University) & P Ajith (Caltech).
Courtesy: S. Dhurandhar
Summary (& next steps?)
THE END
LIGO-Australia: Idea and Opportunity
• The NSF approved grand decision to locate one of
the planned LIGO-USA interferometer detector at
Gingin site, W. Australia to maximize science benefits
like baseline, pointing, duty cycle, technology
development and international collaboration.
• The proposal from Australian consortium envisages
IndIGO as one of the partners to realize this amazing
opportunity.
- Indian contribution in hardware (end station
vacuum system, and controls), Data centre,
manpower for installation and commissioning.
Indo-Aus.Meeting, Delhi, Feb
2011