Transcript IndIGO Indian Initiative in Gravitational

LIGO-India
An Indo-US joint mega-project concept proposal
IndIGO Consortium
(Indian Initiative in Gravitational-wave Observations)
Tarun Souradeep, IUCAA
(Spokesperson, IndIGO)
LIGO Detector at Hanford USA
www.gw-indigo.org
Gravitational waves &
experimental efforts
to detect them!!!
Beauty & Precision
Einstein’s General theory of
relativity is considered the most
beautiful, as well as,
theory of modern physics.
It has matched all weak field
experimental tests of Gravitation in the
solar system remarkably well…
TouTouches everyday Life too…GPS
Einstein’s Gravity predicts
• Matter in motion Space-time ripples; fluctuations in
space-time curvature that propagate as waves
Gravitational waves (GW)
In GR, as in EM, GW travel at the speed of light ,
are transverse and have two states of polarization.
• GW are a major qualitatively unique
prediction beyond Newton’s gravitation
• Any theory of Gravitation consistent with Special Relativity will
lead to GW…However, the properties of GW in different
theories of gravity could be different …
Astrophysical Sources for Terrestrial GW
Detectors
• Compact binary Coalescence: “chirps”
– NS-NS, NS-BH, BH-BH
• Supernovas or GRBs: “bursts”
– GW signals observed in coincidence
with EM or neutrino detectors
• Pulsars in our galaxy: “periodic waves”
– Rapidly rotating neutron stars
– Modes of NS vibration
• Cosmological: “stochastic background” ?
– Probe back to the Planck time (10-43 s)
– Probe phase transitions : window to force
unification
– Cosmological distribution of Primordial black holes
5
Gravitational wave Astronomy :
vit
GWIC Roadmap Document
Era of Advanced LIGO detectors: 2015
10x sensitivity
10x dist reach
 1000 volume
 >> 1000X event
rate
(reach beyond
nearest super-
clusters)
A Day of Advanced
LIGO Observation >>
A year of Initial LIGO
observation
Mean Expected Annual Coalescence Event Rates
Detector
Generation
Initial LIGO
(2002 -2006)
Advanced LIGO
(10X sensitivity)
(2014+ - …)
NS-NS
NS-BH
BH-BH
0.02
0.0006
0.0009
10.
20.0
40
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.
Global Network of GW Observatories improves…
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-India ?
LIGO-Australia?
LIGO-India: a good idea for GW community !
• Geographical relocation Strategic for GW astronomy
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Increased event rates (x2-4) by coherent analysis
Improved duty cycle
Improved Detection confidence
Improved Sky Coverage
Improved Source Location required for multi-messenger astronomy
Improved Determination of the two GW polarizations
• Potentially large Indian science user community in the future
– Indian demographics: youth dominated – need challenges
– Improved UG education system will produce a larger number of students
with aspirations looking for frontline research opportunity at home.
• Substantial data analysis trained faculty exists in India and
Large Data Analysis Center Facilities are being planned under
the next five year plan for consolidated IndIGO participation in
LSC for Advanced LIGO
LIGO-India: Attractive Indian megaproject
• On Indian Soil with International Cooperation (no competition)
• Shared science risks and credits with the International community.
• AdvLIGO setup & initial setup risks primarily rests with USA.
– AdvLIGO-USA precedes LIGO-India by > 2 years.
– Vacuum 10 yr of operation in initial LIGO  2/3 vacuum enclosure + 1/3 detector assembly
split (US ‘costing’ : manpower and h/ware costs)
– Indian expters can contribute to AdvLIGO-USA : opportunity without primary responsibility
• US hardware contribution funded & ready
– AdvLIGO largest NSF project funded in USA
– LIGO-India needs NSF approval, but not additional funds from USA
• Expenditure almost completely in Indian labs & Industry
• Very significant Industrial capability upgrade in India.
• Well defined training plan  Large number of highly trained HRD
• Host a major data analysis facility for the entire LIGO network
LIGO-India: … the opportunity
Science Gain from Strategic Geographical Relocation
Source localization error
Courtesy:
S. Fairhurst
LIGO-India plan
1+1 LIGO USA+ Virgo+ LIGO-India
Original Plan
2 +1 LIGO USA+ Virgo
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: S.Kilmenko & G. Vedovato
LIGO-India: … the opportunity
Strategic Geographical relocation
- the science gain
Sky coverage: ‘reach’ /sensitivity in different directions
Courtesy: Bernard Schutz
LIGO-India: … the challenges
Indian contribution in human resources:
 Trainable Scientific & engineering manpower for detector
assembly, installation and commissioning.
 Trained S & T manpower for LIGO-India sustained
operations for next 10 years.
 Major enhancement of Data Analysis team. Seek
Consolidated IndIGO participation in LIGO Science Collab.
(Sept 2011)
 Expand theory and create numerical relativity simulation.
Expect a significant number of hirings in premier institutions
LIGO-India: … the challenges
Indian contribution in Engineering. &
infrastructure:
 Ultra-high Vacuum enclosure on large scale
 Site (L-configuration: Each 100-200 m x 4.5km: < 300 acres)
 HPC -Data centre
LIGO-India: … the challenges
Indian Site
Requirements:
• Low seismicity
• Low human generated noise
• Air connectivity
• Proximity to Academic institutions, labs, industry preferred, …
• Identify potential sites not too far from existing facilities
• Need to carry out seismic survey to get ground noise
spectral density at 0.1-10 Hz range
• Few interesting possibilities are under investigation
Large scale ultra-high Vacuum
• Fabricated and installed by Indian Industry under close
monitoring by science & technology team
o Oversee the procurement & fabrication of the vacuum system components and its
installation by a national multi-institutional team.
o DAE commitment to LIGO-India  Intense participation of RRCAT & IPR possible.
o All vacuum components such as flanges, gate-valves, pumps, residual gas
analyzers and leak detectors will be bought.
o Companies L&T, Fullinger, HindHiVac, Godrej, … with close support from RRCAT,
IPR and LIGO Lab.
• Preliminary detailed discussions with Industry in Feb 2011 :
Companies like HHV, Fullinger, Godrej in consultation with Stan Whitcomb
(LIGO), D. Blair (ACIGA) since this was a major IndIGO deliverable to LIGOAustralia.
• Preliminary Costing for LIGO-India vacuum component is INR
400 cr. (~80 M USD)
Detector Assembly & Commissioning
For installation and commissioning phase:
• Identify 10-15 core experienced Enggs. & scientists who spend a
year, or more, at Advanced LIGO-USA during its install. & comm.
– LIGO proposal document
– Already 1 IndIGO post-doc at LIGO Caltech, 2 others under consideration in
LIGO and EGO,..
– Creste positions back in India for them (Once project manpower
sanctioned, LIGO-India project hiring at institutions like RRCAT, TIFR, IUCAA,….)
• 6-10 full time engineers and scientists in India.
Present experimental expertise within IndIGO
Laser ITF: TIFR, RRCAT, IITM, IIT K.
UH Vacuum: RRCAT, IPR, (TIFR, IUCNS, new IUCs? )
Each group can scale to 10 Post-doc/PhD students. Over 2-3 years. Train on 3-m prototype .
Concluding Remarks..
Thank you !!!
• Over two decades India has been involved in quality GW research
and been a part of the International GW community
• Since 2009 Indian aspirations involve participation in a major GW
experiment eventually leading to a GW detector in India
• With immense help & encouragement from the International GW
community, IndIGO has made significant progress to integrate
India into the GWIC road map towards the setting up of a Global
GW detector network
• IndIGO is actively pursuing concrete, ambitious, well supported
plans to revamp the scale and scope of Indian participation in GW
research and GW Astronomy in the coming decades.
**All interested researchers are welcome to join our efforts**
LIGO-India: unique once-in-a-generation opportunity
LIGO labs LIGO-India
?
Advanced LIGO Laser
• Designed and contributed by Albert Einstein Institute, Germany
• Much higher power (to beat down photon shot noise)
– 10W
 180W (narrow sub kHz line width)
• Better stability
– 10x improvement in intensity (nano ppm) and frequency
stability (mHz)
• Unique globally. Well beyond current Indian capability. Would require years of
focused R &D effort. Both power and frequency stability ratings.
• AdvLIGO laser has spurred RRCAT to envisage planning development of
similar laser capability in the next 5 year plans. IIT M group also interested.
• Multiple applications of narrow line width laser : Freq time stand, precision
metrology, Quantum key distribution, high sensitivity seismic sensors (geo sc.),
coherence LIDAR (atm sc.), ….
Courtesy: Stan Whitcomb
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Advanced LIGO Mirrors
•
• Larger size
– 11 kg  40 kg, 2534 cm
• Smaller figure error
– 0.7 nm  0.35 nm
• Lower absorption
– 2 ppm  0.5 ppm
• Lower coating thermal noise
Surface specs (/1000) : 100 x best optical telescope
• Surface specs currently available in India for much
smaller sizes /20
Feb 2011 Status
• All substrates delivered • Indian industry may now be challenged to achieve on
small scale, eg., for TIFR 3m prototype
• Polishing underway
• Reflective Coating process• Technology for such mirror useful for high optical
starting up
metrology and other specialized applications
Courtesy: Stan Whitcomb
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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  10 Hz
• Unique design
• New benchmark for isolation experiments in
India : gravitation, Space sensor appls.…
• Application in various industrial and lab test
centers
Courtesy: Stan Whitcomb
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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
– resonance subHz
four stages
– suppression 1/f^4
per stage (6 stages)
40 kg silica test
mass
Courtesy: Stan Whitcomb
25
25
LIGO-India: unique once-in-a-generation opportunity
“Quantum measurements”
to improve further via squeezed light:
• Potential technology spin-offs will impact quantum computing and
quantum key distribution (QKD) for secure communications. (IITM
approached by ITI for QKD development.)
• New ground for optics and communication technology in India
• High Potential to draw
the best Indian UG students, typically
interested in theoretical physics, into experimental science !!!
LIGO-India: … the challenges
Indian contribution in human resources:
 Trained Scientific & engineering manpower for detector
assembly, installation and commissioning (2.)
 Trained SE manpower for LIGO-India sustained operations
for next 10 years (3.)
 Major enhancement of Data Analysis team. Seek
Consolidated IndIGO participation in LIGO Science Collab.
(Sept 2011)
 Expand theory and create numerical relativity simulation.
Expect hiring in premier institutions
Participation in LSC during Advanced LIGO
Proposed Data Analysis activities of the IndIGO Consortium
•Principal Leads: K.G. Arun, R.Nayak, A. Pai, A. Sengupta, S. Mitra
• Participants: S. Dhurandhar, T. Souradeep, B. R. Iyer, C.K. Mishra,
M.K. Harris,….
• Institutions: CMI, IUCAA, IISER (Kolkata), IISER (Tvm), Univ Delhi
•Projects
• Multi-detector Coherent veto
•Tests of GR and alternative theories of gravity
•Stochastic Gravitational wave background analysis
• IndIGO Data Center
IndIGO Data Centre
@
IUCAA
Anand Sengupta, DU, IndIGO
 Primary Science: Online Coherent search for GW signal from
binary mergers using data from global detector network
Coherent  2-4 x event rate (40  80-160 /yr for NS-NS)
 Role of IndIGO data centre
 Large Tier-2 data/compute centre for archival of GW data and analysis
 Bring together data-analysts within the Indian gravity wave community.
 Puts IndIGO on the global map for international collaboration with LIGO
Scientific Collaboration. Facility for LSC as part of IndIGO participation.
 Large University sector participation via IUCAA
• 200 Tflops peak capability (by 2014)
• Storage: 4x100TB per year per interferometer.
• Network: gigabit+ backbone, National Knowledge Network
• Gigabit dedicated link to LIGO lab Caltech
• 20 Tf 200 Tb funded by IUCAA : ready Mid 2012
Indo-US centre for Gravitational Physics and
Astronomy @ IUCAA
APPROVED (Dec 2010). Funds received Jul 6, 2011
• Centre of Indo-US Science and Technology Forum (IUSSTF)
• Exchange program to fund mutual visits and facilitate
interactions leading to collaborations
• Nodal centres: IUCAA , Pune, India & Caltech, Pasadena, USA.
• Institutions:
Indian: IUCAA, TIFR, IISER, DU, CMI - PI: Tarun Souradeep
USA: Caltech, WSU
- PI: Rana Adhikari
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
Courtesy:
Precision
Bernard Schutz
High precision experimental expertise in India
• TIFR : High precision experiments and tests of weak forces
[C.S. Unnikrishnan]
– Test gravitation using most sensitive torsional balances and optical sensors.
– Techniques related to precision laser spectroscopy, electronic locking, stabilization.
– G.Rajalakshmi (IIA  TIFR, 3m prototype);
– Suresh Doravari (IIA  LIGO, Caltech 40m/Adv LIGO)
• RRCAT (RR Center for Advanced Tech.)
– [S.K. Shukla on INDUS, A.S. Raja Rao (ex RRCAT)] --UHV
– [Sendhil Raja, P.K. Gupta] - Optical system design, laser based
instrumentation, optical metrology, Large aperture optics, diffractive optics,
micro-optic system design.
– [Rijuparna Chakraborty, France  LIGO/EGO pdf?] Adaptive Optics….
• IPR (Institute for Plasma Research)
– [S.B. Bhatt on Aditya and Ajai Kumar] - UHV , Lasers, Control systems,..
• IITM [Anil Prabhakar] and IITK [Pradeep Kumar] (EE depts)
–
–
Photonics, Fiber optics and communications
Characterization and testing of optical components and instruments for use in India..
Large experiment expertise in India
• Groups at BARC (Bhabha Atomic Res. Center) and RRCAT : involved
in LHC hardware contribution
– provided a variety of components and subsystems like precision magnet positioning stand
jacks, superconducting correcting magnets, quench heater protection supplies and skilled
manpower support for magnetic tests and measurement and help in commissioning LHC
subsystems.
• Teams at Electronics & Instrumentation Groups at BARC
(may be interested in large instrumentation projects in XII plan)
• IPR
(Inst. for Plasma res.): Involved in ITER (6xLIGO-Ind cost)
Support role in large volume UHV system, Control systems,….
• Groups at ISRO (Ind. Space Res. Org.) ,…….
Control systems, Clean rooms, Large scale fabrication, ......
• Over the last two years contacts made with the above
groups  opportunities in a GW experiment and
explore their possible participation in LIGO-India/Aus.
Multi-Institutional,
Multi-disciplinary Consortium
(Aug. 2009)
Nodal Institutions
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3.
4.
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6.
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9.
10.
CMI, Chennai
Delhi University
IISER Kolkata
IISER Trivandrum
IIT Madras (EE)
IIT Kanpur (EE)
IUCAA, Pune
RRCAT, Indore
TIFR, Mumbai
IPR, Bhatt
Others
•
•
•
RRI
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.
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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
Bhal Chandra Joshi NCRA, Pune
Rijuparna Chakraborty, Cote d’Azur, Grasse
Rana Adhikari
Caltech, USA
Suresh Doravari
Caltech, USA
Biplab Bhawal
(ex LIGO)
Sunil
(IPR/UWA)
RRI, Bangalore
IUCAA, Pune
TIFR, Mumbai
IUCAA, Pune
1.
2.
3.
4.
5.
6.
7.
8.
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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
Sanjay Sahay
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 .
BITS, Goa
Caltech , USA
Wash. U., USA
Cardiff University, UK
UTB, Brownsville , USA
Max Planck AEI, Germany
IndIGO: Goals & current activities
• Provide a common umbrella to initiate and expand GW
related experimental activity and train new technically skilled
manpower
• Seeking pan-Indian consolidated IndIGO membership in LIGO
Scientific Collaboration (LSC) for participation in Advanced LIGO.
• Create a Tier-2 data centre in IUCAA for LIGO Scientific
Collaboration Deliverables and as a LSC Resource
 Starting collaborative work under the IUSSTF Indo-US
IUCAA-Caltech joint Centre at IUCAA
 Indo-Jap project “Coherent multi-detector gravitational wave
search using LCGT and advanced interferometers”
 Explore the Roadmap for EGO-IndIGO collaboration on GW and a
possible MOU (Meeting on Nov 1-2 ,2011 at IUCAA)
 Explore Indian participation in LISA and space based GW detectors
in the future ( ASTROD 5 meeting on July 14 – 16, 2012 at RRI)
IndIGO Consortium – a brief history
• Dec. 2007 : ICGC2007 @IUCAA: Rana Adhikari’s visit & discussions
• 2009:
– Australia-India S&T collaboration (Iyer & Blair)
Establishing Australia-India collaboration in GW Astronomy
–
IndIGO Consortium: Reunion meeting IUCAA (Aug 9, 2009)
–
GW Astronomy Roadmap for India;
• 2009-2011:
– Meetings at Kochi, Pune, Shanghai, Perth, Delhi
to Define, Reorient and Respond to the Global (GWIC) strategies
for setting up the International GW Network.
– Bring together scattered Indian Experimental Expertise;
Individuals & Institutions
• March 2011: IndIGO-I Proposal: Participation in LIGO-Australia
• May 2011+: LIGO-India..
IndIGO: the Aspiration
• Create major Indian presence in GW astronomy
 MOU with ACIGA to collaborate on GW
Astronomy
 Partner in LIGO-Australia
– Indian partnership at 15% of Australian cost with full data rights
A significant recent development …
LIGO-India
– Letter from LIGO Lab. with a concept proposal for LIGO-India
 LIGO-India is under preliminary consideration for National
Mega Projects under the forthcoming Five year plan in
India .
RRCAT (Next Plan period): Advanced Interferometry
(Narrow line width Frequency Stabilised laser development)
The laser will be an injection seeded Nd;YAG or Yb:Silica fiber laser locked to a stabilized reference
cavity. The target would be to demonstrate a laser with 1W output and sub-kHz line width and few Hz
stability. Scaling up of the power to 10W will be done as the next step.
RRCAT: Advanced Interferometry
(Ultraflat Components development)
Development of Ultraflat Optical
components such as mirrors for GWD will
require augmenting the existing facility with
an ion beam figuring system for final
correction of the polished optics to /500
or better.
Photonics @ IIT-Madras (& IIT- Kanpur)
11 faculty members (8 in EE, 3 in Physics)
10 M. Tech scholars in EE (Photonics)
20+ research scholars (M.S. and Ph.D.)
Research specializations
➲ Optical communications
➲ Fiber lasers
➲ Diffractive optical elements
➲ Silicon photonics, plasmonics
➲ Nonlinear and quantum optics
IndIGO 3m Prototype Detector
Funded by TIFR Mumbai on campus (2010)PI: C. S.Unnikrishnan ( INR 3.5cr ~.7 M$ )
Goals of the TIFR 3-m prototype interferometer (to be operational in 2014):
1) Research and Training platform with all the features of the
advanced LIGO-like detectors, scaled down to displacement
sensitivity around 10-18 m, above 200 Hz.
2) The Indian research platform for features like signal
recycling, DC read-out, and most importantly the use of
squeezed light and noise reduction (last phase).
3) Instrument for studies on short range gravity and QED force,
especially a measurement of the Casimir force in the range
10 -100 microns where no previous measurements exist
(Rajalakshmi and Unnikrishnan, Class, Quant. Grav. 27, 215007 (2010).
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 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
Gravitational wave Astronomy :
vit
Synergy with other major Astronomy projects
• SKA : Pulsars timing and GW background, GW from Pulsars ,…
( RADIO: Square Kilometer array)
• CMB : GW from inflation, cosmic phase transitions, dark energy ….
(Cosmic Microwave Background : WMAP, Planck, CMBPOl, QUaD,…)
• X-ray satellite (AstroSat) : Spacetime near Black Holes, NS, ….
• Gamma ray observatory: GRB triggers from GW
(FermiLAT, GLAST,….)
• Thirty Meter Telescope: Resolving multiple AGNs, optical follow-up, …
• INO: cross correlate neutrino signals from SN event
• LSST: Astro-transients with GW triggers, Cosmic distribution of dark
matter , Dark energy
•
•
GWIC Roadmap Document