The IndIGO Project

IAGRG, HRI, Allahabad 20th January 2011

The IndIGO Project

Sanjeev Dhurandhar


Formation of the consortium for IndIGO

People from several important institutes have come together

to form a consortium – TIFR, RRI, IUCAA, CMI, DU, IISERs, …

The aim of the consortium is to promote and foster

Indian Initiative in Gravitational Wave Astronomy

Set up the roadmap and a phased strategy towards the

Indian Interferometric Gravitational-wave Observatory (IndIGO)


International Network of GW Interferometers

LIGO-LLO: 4km

LIGO-LHO: 2km, 4kmGEO: 0.6km VIRGO: 3km

TAMA: 0.3km

AIGO: (?)km

1. Detection confidence 2. Source direction 3. Polarisation info


The Road Map for IndIGO

3 metre scale prototype : Current

C. S. Unnikrishnan & group at T.I.F.R.

Collaboration with LIGO - Australia: Current

Ranjan Gupta (IUCAA), Ajai Kumar (IPR),

Unnikrishnan (TIFR), RRCAT

IndIGO document submitted to directors + other VIP

Members of IndIGO consortium


1. S. V. Dhurandhar (IUCAA)2. B. R. Iyer (RRI)3. C. S. Unnikrishnan (TIFR)4. T. Souradeep (IUCAA)5. R. Adhikari (LIGO-Caltech)6. B. S. Sathyaprakash (Cardiff)7. K. G. Arun (CMI)8. B. Bhawal (USA)9. S. Bose (WSU)10. P. Dasgupta (DU)11. S. Doravari (LIGO-Caltech)12. A. Gopakumar (TIFR)13. R. Gupta (IUCAA)14. S. Jhingan (Jamia Millia)15. B. Krishnan (AEI)16. A. Kumar (IPR)

17. S. Mitra (JPL-LIGO)18. S. Mohanty (UTB)19. R. Nayak (IISER)20. A. Pai (IISER)21. A. Parmeswaran (LIGO-Caltech)22. G. Rajalakshmi (TIFR)23. T. Seshadri (DU)24. A. Sengupta ( DU)

International Advisory Committee


1. Rana Adhikari (LIGO, Caltech)2. David Blair (UWA)3. A. Giazotto (Virgo, Italy)4. P. D. Gupta (RRCAT)5. Jim Hough (GEO, Glasgow)6. K. Kuroda (LCGT, Japan)7. H. Lueck (GEO, Hannover)8. Nary Man (Virgo, France)9. Jay Marx (LIGO, director)10. David McClelland (ANU)11. Jesper Munch (ACIGA, Chair)12. B. S. Sathyaprakash (Cardiff)13. B. F. Schutz (AEI director, GEO)14. J-Y. Vinet (Virgo, France)15. Stan Whitcomb (LIGO, Caltech)

Organisation & Sub-committees


Council

AIGO deliverables

3 m prototype

LSC IndIGOhomepage

Workshops Schools

Communication Documentation

The sub-committees


• Council: B. Iyer (Chair), S. Dhurandhar (spokesperson), C. S. Unnikrishnan & T. Souradeep

• 3 metre: C. S. Unnikrishnan, G. Rajalakshmi & S. Doravari

• AIGO deliverables: A. Kumar, R. Gupta & C. S. Unnikrishnan

• LSC related: S. Dhurandhar, A. Pai & R. Nayak

• IndIGO homepage: A. Sengupta, S. Mitra, A. Parmeswaran , K. G. Arun & T. Souradeep

• Workshops/Schools: T. Souradeep, T. Seshadri, Gopakumar, R. Nayak & A. Pai

• Communications: same as IndIGO homepage

The 3 metre prototype


People: Unnikrishnan (PI), Rajalakshmi, Jorge Fiscina

Time-scale: 2 ½ years

Budget: 0.6 million USD ~ Rs. 26,000,000 - FUNDED

Laboratory: TIFR, Mumbai to be shifted later to a quieter place Hyderabad/Pune.

Objectives: Manpower training, measurements related to short- range forces and Newtonian gravity.

Instrument: 3 m arm-length Michelson interferometer with Fabry- Perot enhancement.

Sensitivity: In actual operation ~ 5x10-18 m/√Hz above 200 Hz (not aiming for theoretical minimum).

Indo-US centre for Gravitational Physics and Astronomy


• Project of Indo-US Science and Technology Forum

• 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

APPROVED/FUNDED !

Key aspects of vacuum and control systems for LIGO Australia


• MOU with Australia signed

• People: Ranjan Gupta, Ajai Kumar & C. S. Unnikrishnan, A. S. Raja Rao (formerly CAT)

• Feasibility and cost estimate on the basis of LIGO system is being worked out with Hind High Vacuum company, Bangalore.

• Meeting in Delhi with LIGO and Australians in February 2011 to plan the future steps and deliverables from India

• Indo-Australian exchange grant: Unnikrishnan & Blair

Manpower Training: IndIGO school at Delhi IRC


GRAND SUCCESS!IndIGO school on Gravitational Wave Astronomy held at Delhi University from 13-24 December 2010.

• Coordinators: Seshadri & Sengupta + SVD

• Theory, Data Analysis & Experiment

• Lecturers included: Alan Weinstein (Caltech) B. S. Sathyaprakash (Cardiff) C. S. Unnikrishnan (TIFR) SVD (IUCAA)

• Students from IITs, IISERs, Universities

• IndIGO summer internships at international GW laboratories: 6 students Caltech, UTB (2010) – plans to include other groups

The first IndIGO School



30 metre class prototype: 2014-2015 (?)

Advanced detector IndIGO: 2020+

Future Directions

Vacuum tanksDetector

Laser table

Vibration isolationschematic

All mirros and beamsplitters are suspended as in the diagram on right

3.2 meters

0.8 mF-P cavityPower recycling

Sensing &Control

60 cm

180 cm

Mirror

6 m6 m

Frequency (Hz)

1 10 100 1000

10-20

10-19

10-18

10-17

10-16

10-15

10-14

Shot noise

Seismic (best and worst case, dashed)

( / )l m Hz

10000Signal recycling + Squeezing

Something worth progressing to…

SQL

Sketch of expected sensitivity for 3-m prototype

Best case total

suspension noise

The Experimental Program: Road Map

1) 3 meter scale prototype interferometer with power recycling and displacement sensitivity of 10-18 m/√Hz above 300 Hz

Funded (TIFR)(2011-14)

2) Add signal recycling and squeezed light to match the best of prototypes

Funded (2015)

3) Leverage Indo-US and Indo-Australian exchange programs to develop specific expertise in vibration isolation, optical cavities and data handling techniques

Indo-US funded (2011-2014)Indo-Aus. under review

4) Project proposal (Rs. 130 Crores over 8 years) being prepared for participation in LIGO-Australia (participation in vacuum systems, control systems, data handling and data analysis, part from tests and validation). Detector to be built during 2012-2017 with LIGO components and design

To be submitted synchronous with Australian proposal to their Govt. this year.

5) Envisage a vigorous GW detection and astronomy program after 6-8 years. But more people to get interested and volunteer for the experimental program.

Will also aid in experiments in short range gravity and Casimir force measurements with unprecedented sensitivity: (G. Rajalakshmi and CS Unnikrishnan, CQG, 2011)


Features: 1) 3 m arm-length Michelson interferometer with Fabry-Perot enhancement, mirror

size of 15 cm.2) Finesse of F-P cavity ~ 3003) Laser power input: ~ 1 W, frequency and amplitude stabilized NPRO Nd:YAG

laser or Fiber amplifier enhanced seed NPRO. 4) Power recycling: Yes5) Signal recycling: to be decided6) Squeezed light: Planned for later (part of the training feature, will be developed

and implemented separately in our optics lab).7) Vibration isolation: Passive 3-stage, to reach <10-18 m above 200 Hz.8) Vacuum: 10-8 mbar, 3 ion pumps and NEG pumps.9) Mode cleaner: Fiber based.10) Sensitivity in actual operation ~ 5x10-18 m/√Hz above 200 Hz (not aiming for

theoretical minimum). 11) Time scale for completion: 2.5 years12) Laboratory: TIFR, Mumbai, to be shifted to a quieter place later (Hyderabad or

Pune).13) Budget (hopeful, in 2010): ~ 0.6 million US$14) Applications: Training, and measurements related to short-range forces and

Newtonian gravity.

The IndIGO Project

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