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The IndIGO Project

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

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The IndIGO Project

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  1. The IndIGO Project SanjeevDhurandhar IAGRG, HRI, Allahabad 20th January 2011

  2. 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 InterferometricGravitational-wave Observatory (IndIGO) IAGRG, HRI, Allahabad 20th January 2011

  3. GEO: 0.6km VIRGO: 3km LIGO-LHO: 2km, 4km TAMA: 0.3km LIGO-LLO: 4km AIGO: (?)km International Network of GW Interferometers 1. Detection confidence 2. Source direction 3. Polarisation info IAGRG, HRI, Allahabad 20th January 2011

  4. 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 • IndIGOdocument submitted to directors + other VIP IAGRG, HRI, Allahabad 20th January 2011

  5. Members of IndIGO consortium • S. V. Dhurandhar (IUCAA) • B. R. Iyer (RRI) • C. S. Unnikrishnan (TIFR) • T. Souradeep (IUCAA) • R. Adhikari(LIGO-Caltech) • B. S. Sathyaprakash (Cardiff) • K. G. Arun(CMI) • B. Bhawal (USA) • S. Bose (WSU) • P. Dasgupta (DU) • S. Doravari(LIGO-Caltech) • A. Gopakumar (TIFR) • R. Gupta (IUCAA) • S. Jhingan (JamiaMillia) • B. Krishnan (AEI) • A. Kumar (IPR) • S. Mitra(JPL-LIGO) • S. Mohanty (UTB) • R. Nayak (IISER) • A. Pai (IISER) • A. Parmeswaran(LIGO-Caltech) • G. Rajalakshmi (TIFR) • T. Seshadri (DU) • A. Sengupta(DU) IAGRG, HRI, Allahabad 20th January 2011

  6. International Advisory Committee • Rana Adhikari (LIGO, Caltech) • David Blair (UWA) • A. Giazotto (Virgo, Italy) • P. D. Gupta (RRCAT) • Jim Hough (GEO, Glasgow) • K. Kuroda (LCGT, Japan) • H. Lueck (GEO, Hannover) • Nary Man (Virgo, France) • Jay Marx (LIGO, director) • David McClelland (ANU) • Jesper Munch (ACIGA, Chair) • B. S. Sathyaprakash (Cardiff) • B. F. Schutz (AEI director, GEO) • J-Y. Vinet (Virgo, France) • Stan Whitcomb (LIGO, Caltech) IAGRG, HRI, Allahabad 20th January 2011

  7. Organisation & Sub-committees AIGO deliverables 3 m prototype IndIGO homepage LSC Council Workshops Schools Communication Documentation IAGRG, HRI, Allahabad 20th January 2011

  8. 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 IAGRG, HRI, Allahabad 20th January 2011

  9. 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). IAGRG, HRI, Allahabad 20th January 2011

  10. Indo-US centre for Gravitational Physics and Astronomy APPROVED/FUNDED ! • 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: TarunSouradeep • US: Caltech, WSU - PI: RanaAdhikari IAGRG, HRI, Allahabad 20th January 2011

  11. 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 IAGRG, HRI, Allahabad 20th January 2011

  12. Manpower Training: IndIGO school at Delhi IRC • GRAND SUCCESS! • IndIGOschool 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 IAGRG, HRI, Allahabad 20th January 2011

  13. The first IndIGO School IAGRG, HRI, Allahabad 20th January 2011

  14. Future Directions • 30 metre class prototype: 2014-2015 (?) • Advanced detector IndIGO: 2020+ IAGRG, HRI, Allahabad 20th January 2011

  15. 6 m 6 m

  16. Seismic (best and worst case, dashed) Signal recycling + Squeezing Something worth progressing to… Sketch of expected sensitivity for 3-m prototype 10-14 10-15 Best case total 10-16 10-17 SQL suspension noise 10-18 10-19 Shot noise 10-20 1 100 1000 10000 10 Frequency (Hz)

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

  18. Features: • 3 m arm-length Michelson interferometer with Fabry-Perot enhancement, mirror size of 15 cm. • Finesse of F-P cavity ~ 300 • Laser power input: ~ 1 W, frequency and amplitude stabilized NPRO Nd:YAG laser or Fiber amplifier enhanced seed NPRO. • Power recycling: Yes • Signal recycling: to be decided • Squeezed light: Planned for later (part of the training feature, will be developed and implemented separately in our optics lab). • Vibration isolation: Passive 3-stage, to reach <10-18 m above 200 Hz. • Vacuum: 10-8 mbar, 3 ion pumps and NEG pumps. • Mode cleaner: Fiber based. • Sensitivity in actual operation ~ 5x10-18 m/√Hz above 200 Hz (not aiming for theoretical minimum). • Time scale for completion: 2.5 years • Laboratory: TIFR, Mumbai, to be shifted to a quieter place later (Hyderabad or Pune). • Budget (hopeful, in 2010): ~ 0.6 million US$ • Applications: Training, and measurements related to short-range forces and Newtonian gravity. IAGRG, HRI, Allahabad 20th January 2011

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