Presentation on theme: "IAGRG, HRI, Allahabad 20th January 2011. Formation of the consortium for IndIGO People from several important institutes have come together to form."— Presentation transcript:
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)
IAGRG, HRI, Allahabad 20th January 2011 International Network of GW Interferometers International Network of GW Interferometers LIGO-LLO: 4km LIGO-LHO: 2km, 4km GEO: 0.6km VIRGO: 3km TAMA: 0.3km AIGO: (?)km 1. Detection confidence 2. Source direction 3. Polarisation info
IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 Council AIGO deliverables 3 m prototype LSC IndIGO homepage Workshops Schools Communication Documentation
The sub-committees IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011 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 IAGRG, HRI, Allahabad 20th January 2011
30 metre class prototype: 2014-2015 (?) Advanced detector IndIGO: 2020+ Future Directions
Frequency (Hz) 1 10 1001000 10 -20 10 -19 10 -18 10 -17 10 -16 10 -15 10 -14 Shot noise Seismic (best and worst case, dashed) 10000 Signal 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)
IAGRG, HRI, Allahabad 20th January 2011 Features: 1)3 m arm-length Michelson interferometer with Fabry-Perot enhancement, mirror size of 15 cm. 2)Finesse of F-P cavity ~ 300 3)Laser power input: ~ 1 W, frequency and amplitude stabilized NPRO Nd:YAG laser or Fiber amplifier enhanced seed NPRO. 4)Power recycling: Yes 5)Signal recycling: to be decided 6)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 years 12) 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.