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Towards Detection of Gravitational Waves 1.5 A1B1G1 A3B3G1 1 TAMA A4B1G2 ] Burst –20 0.5 Search

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Towards Detection of Gravitational Waves 1.5 A1B1G1 A3B3G1 1 TAMA A4B1G2 ] Burst –20 0.5 Search Towards Detection of Gravitational Waves 1.5 A1B1G1 A3B3G1 1 TAMA A4B1G2 ] Burst –20 0.5 Search 0 –0.5 Barry C. Barish Amplitude [x 10 –1 Gravitational waveforms from stellar–core collapse Caltech (10kpc from the earth) –1.5 0 1020304050 Time [msec] GR-17 20-July-04 Towards Detection of Gravitational Waves From Bars Bars with Increased Bandwidth Spheres From Interferometers Advanced Interferometers Next Generation (QND) Detectors From 6 Mpc (NN inspiral) 200 Mpc and then beyond From Upper Limits Searches Detections From Generic Searches Searches using Specified Waveforms From Single Detectors Global Networks 20-July-04 GR-17 - Barish 2 Resonant Bar MiniGrail Auriga, Italy The Netherlands Detectors Allegro USA Schenberg Brazil Nautilus, italy Explorer Switzerland Niobe 20-July-04 GR-17 - Barish Australia 3 Network of Resonant Bars Allegro Explorer Auriga Nautilus Niobe IGEC Network 20-July-04 GR-17 - Barish 4 International Gravitational Event Collaboration (IGEC) ALLEGRO,AURIGA,EXPLORER, NAUTILUS, and NIOBE 1997-2000. The search for burst waves at resonant frequency ~ 900 Hz. The detectors nearly parallel to maximize coincident sensitivity. Candidate events at SNR > 3-5 (~ background events 100/day) Data exchanged: peak amplitude, time of event and uncertainties. Threshold equivalent to ~0.1 M⊙ converted into a gravitational wave millisecond burst at a distance of 10 kpc. The accidental coincidence rate over 1 sec interval (e.g. bandwidth of 1 Hz) was ~ few/week two-fold and ~few/century three-fold. Time resolution not sufficient to resolve incident wave direction, no directional search has been applied. No evidence for grav wave bursts was found. 20-July-04 GR-17 - Barish 5 IGEC coincidence search Upper Limit on the Rate of gravitational waves bursts from the GALACTIC CENTER random arrival times and amplitude ≥ search threshold h Final results 1.E+03 IGEC rate 1.E+02 [y –1] The Area above the blue curve is excluded with a coverage > 90% 1.E+01 1.E+00 1E-18 1E-17 1E-16 search threshold h -18 h ~ 2 10 ∆E ~ 0.02 M⊙ converted @ 10 kpc 20-July-04 [P. Astone, et al. GR-17 Phys. - BarishRev. D68 (2003) 022001] 6 LIGO Louisiana TAMA Japan 4000m 300m Interferometer Detectors Virgo Italy 3000m GEO Germany AIGO Australia 600m future LIGO Washington 2000m & 4000m 20-July-04 GR-17 - Barish 7 Network of Interferometers LIGO GEO Virgo TAMA decompose the polarization of AIGO detectiongravitationallocate the confidence sources waves 20-July-04 GR-17 - Barish 8 Gravitational Wave Detection free masses h = strain amplitude of grav. waves h = ∆L/L ~ 10-21 Cylindrical Spherical Resonant Suspended(future) L = 4 Barskm mass Interferometers ∆L ~ 10-18 m 20-July-04 GR-17 - Barish 9 AURIGA LHe4 vessel Al2081 holder Electronics wiring support Main Attenuator Thermal Sensitive bar Shield Compression Spring 20-July-04 GR-17 - Barish Transducer 10 The resonant transducer The displacement of the secondary oscillator modulates a dc electric or magnetic field or the frequency of a s.c. cavity xM xm 20-July-04 GR-17 - Barish 11 Sensitivity of Resonant Detectors Noise in the detector Extrinsic: Seismic noise ⇒ mechanical filter Intrinsic: Thermal noise ⇒ cool detector amplifier noise ⇒ SQUID amplifier amplifier transducer 20-July-04 GR-17 - Barish 12 EXPLORER 2 ton Al bar 3m long 0.6 m diameter 1998 2001 2003 20-July-04 GR-17 - Barish 14 EXPLORER The noise temperature is < 3 mK (h = 4.4 10-19) for 84% of the time. The peak strain sensitivity is 10-21/√Hz and the bandwidth 30 Hz @ 10-21/√Hz Cosmic ray detectors installed Improved Bandwidth and Duty Cycle > 90% (2004) 20-July-04 GR-17 - Barish 15 Nautilus Aluminum Bar vs = 5400 m/s Length = 3meter Mass = 2300kg Freq ~900 Hz 20-July-04 GR-17 - Barish 16 NAUTILUS 2003 • New bar tuned f = 935 Hz • New suspension cable • New capacitive transducer • Quantum Design dc SQUID Bar cooled 3.5 K April 2003 Peak strain sensitivity 2 x 10-21/√ Hz Bandwidth 30 Hz @10-20/√ Hz 20-July-04 GR-17 - Barish 17 NAUTILUS 2004 Duty cycle > 90% Tnoise in 2001 Example: 100 hours in june 2004 - 1 minute averages All samples are below 1.4 mK <Tnoise> = 628 mK 20-July-04 GR-17 - Barish 18 NAUTILUS 10 -17 10 -18 Spectral density at 3.5 K June 2003 10 -19 10 -20 Strai sensitivity (Hz^-1/2) -21 10 -21 2*10 -22 10 -17 860 880 900 920 940 960 980 1000 10 frequency (Hz) 10 -18 2001 10 -19 Expected spectral density 10 -20 at 0.15 K Strai sensitivity (Hz^-1/2) 10 -21 -22 6*10 -22 -2210 1.6*10 860 880 900 920 940 960 980 1000 frequency (Hz) 20-July-04 GR-17 - Barish 19 EXPLORER-NAUTILUS 2001 During 2001 EXPLORER and NAUTILUS were the only two operating resonant detectors, with the best ever reached sensitivity. An algorithm based on energy compatibility of the event was applied to reduce the “background”Excess ??? Direction of Galactic Disc events Number of Sidereal hours ROG Coll.: CQG 19, 5449 (2002) L.S.Finn: CQG 20, L37 (2003) P.Astone,New G.D’Agostini, data S.D’Antonio: is CQG needed Proc. Of GWD AwithW 2002, gr-qc/0304096 more E. Coccia ROG Coll.:CQG Proc. Of GWDAW 2002 ROG Coll.: gr-qc/0304004antennas in coincidence ! 20-July-04 GR-17 - Barish 20 Auriga L = 3 m M = 2000 kg F ~ 900 Hz T ~ 150 mK 20-July-04 GR-17 - Barish 21 AURIGA 2nd run: preliminary results * * * * * * _ Experimental results _ Expected sensitivity Spurious lines (x) are related to environmental noise but do not affect Best result obtained when significantly the burst sensitivity e.g., spurious lines fade out for a 1 ms sin-gaussian pulse: -19 hmin≈ 3 x10 in both situation Bandwidth: h < 5x10-21 Hz-1/2 within ~100 Hz band (noise floor) 20-July-04 GR-17 - Barish 22 NIOBE (discontinued operation) Parametric transducer Nb bar with m=1500 kg, f~700 Hz T~5.5K h~3x10-19 20-July-04 GR-17 - Barish 23 ALLEGRO Calculated sensitivity: -20 5 ∆f~100 Hz h ~ 7.6x10 TN ~1.3x10 K 20-July-04 GR-17 - Barish 24 ALLEGRO Antenna mass =1150 Kg (Al) Q=9x106 @ 4.4K ∆f ~ 100 Hz h ~ 7.6 x 10-20 20-July-04 GR-17 - Barish 25 ALLEGRO Transducer Transducer built by the Maryland group H.J.Paik, H.Vol Moody and A.Weber (Proc. Amaldi-5 conference 2003) 20-July-04 GR-17 - Barish 26 Astrophysical Sources Compact binary inspiral: “chirps” » NS-NS waveforms are well described » BH-BH need better waveforms » search technique: matched templates Supernovae / GRBs: “bursts” » burst signals in coincidence with signals in electromagnetic radiation » prompt alarm (~ one hour) with neutrino detectors Pulsars in our galaxy: “periodic” » search for observed neutron stars (frequency, doppler shift) » all sky search (computing challenge) » r-modes Cosmological Signals “stochastic background” 20-July-04 GR-17 - Barish 27 ALLEGRO - LIGO Livingston Bar- Interferometer Combined Search for Stochastic Signals See McHugh 40 km Separation Rotate Bar Modulating the experimental signature of a stochastic gravitational wave background, Finn and Lazzarini Phys. Rev. D 64, 082002 (2001) 20-July-04 GR-17 - Barish 28 Resonant Spheres The future?? TIGA • Much larger cross-section than a bar of the same resonant frequency (up to 70 x) • Omni-directional: Allows for the determination of direction and polarization • Require 6 transducers • Hollow spheres could allow a choice of cross-sections and frequencies 20-July-04 GR-17 - Barish 29 MiniGrail (Leiden) Material CuAl6% Density ρ = 8000 kg/m3 Diameter Φ = 0.68 m Mass M = 1100 kg Sound vel v = 4000 m/s Res. freq. f = 3160 Hz T-sphere T = 78 mK Recent Improvements (2004): Larger sphere (1100 ⇒ 1300 kg) Improved attenuation (30 dB ⇒ 50 dB) 3 Capacitive transducers Double stage SQUID amplifier 700 hbar 20-July-04 GR-17 - Barish 30 MiniGRAIL sensitivity MiniGRAIL run 6 MiniGRAIL NAUTILUS/EXPLORER run 7 Planned at GEO the end of 2004 AURIGA LIGO S3 Initial target large interferometers 20-July-04 GR-17 - Barish 31 Mario Schenberg (Brazil) Assembled and cooled to 2 K Three-mode parametric transducer m1=1150 Kg; m2=53g; m3=0.01g Expected sensitivity with this system H = 2 10-21√Hz ; 50Hz bandwidth 20-July-04 GR-17 - Barish 32 Large Hollow Sphere possibly underground - R&D in progress by ROG Detection of collapses and chirps @ 200Mpc; -8 Stochastic Background : Ωgw~ 10 D = 4.8 m; f1=300 Hz; Hollow Sphere 1st and 2nd modes f2=1000 Hz; SQL readout 20-July-04 GR-17 - Barish 33 Nested Resonant Masses AURIGA Sensitive in a kHz-wide frequency band Mo Dual 16.4 ton height 2.3 m Ø 0.94m SiC Dual 62.2 ton height 3 m Ø 2.9m T~0.1 K , Standard Quantum Limit flat sensitivity in a wide band 20-July-04 GR-17 - Barish 34 Suspended Mass Interferometer Projects Interferometer Concept Laser used to measure Arms in LIGO are 4km relative lengths of two Measure difference in orthogonal arms length to one part in 1021 or 10-18 meters …causing the interference pattern As a wave to change at the Suspendedpasses, the photodiode armMasses lengths change in different ways…. 20-July-04 GR-17 - Barish 36 TAMA Past data taking (DT) Period Obs. Time Main Target DT1 1999 8/6～8/7 11h Establishment of calibration DT2 1999 9/17～9/20 31h First event search DT3 2000 4/20~4/23 13h Improved sensitivity DT4 2000 8/21~9/4 167h 100-h data DT5 2001 3/2~3/10 111h 24-h full-time observation DT6 2001 8/1~9/20 1038h 1000-h data DT7 2002 8/31~9/2 25h Recycling DT8 2003 2/14~4/15 1158h International coincidence run DT9 2003/4 11/28~1/10 557h Automatic operation 20-July-04 GR-17 - Barish 37 TAMA Sensitivity in DT9 Recycling gain: 4.5 Extended control band width for the laser frequency Improved strain sensitivity: h=1.7x10-21 /Hz1/2 @1kHz 20-July-04 GR-17 - Barish 38 Astrophysical Sources Compact binary inspiral: “chirps”
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