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Amaldi-6 Caltech 24-June Barry C Final Thoughts and Highlights Barry C. Barish LISA Caltech Amaldi-6 Okinawa 24-June -05 Towards Detection of Gravitational Waves From LISA Concept Demonstrations Mission From Bars Bars with Increased Bandwidth Spheres From Interferometers Advanced Interferometers Next Generation (QND) Detectors From 8 Mpc (NN inspiral) 200 Mpc and then beyond From Upper Limits Searches Detections From Generic Searches Searches with Specified Waveforms From Single Detectors Global Networks 24-June-05 Amaldi-6 - Barish 2 Gravitational Waves in Space LISA Three spacecraft, each with a Y-shaped payload, form an equilateral triangle with sides 5 million km in length. 24-June-05 Amaldi-6 - Barish 3 LISA 24-June-05 Amaldi-6 - Barish 4 LISA 24-June-05 Amaldi-6 - Barish 5 LISA 24-June-05 Amaldi-6 - Barish 6 WD-WD, WD-NS, NS-NS binaries with GW frequency within LISA band are observed. These sources are GUARANTEED Distribution of WD binaries (Nelemans et al) Total number of detatched binaries Total number of interacting binaries 208736473 34291253 24-June-05 Amaldi-6Krolak - Barish 7 Data Analysis Issues Stochastic Interacting Isolated signals signal signals TDI Long wavelength regime Short wavelength regime LISA motion; long observation times; network of detectors 24-June-05 Amaldi-6Krolak - Barish 8 LISA 24-June-05 Amaldi-6 - Barish 9 LISA The diagram shows the sensitivity bands for LISA and LIGO 24-June-05 Amaldi-6 - Barish 10 24-June-05 -1/2 Strain [Hz ] DECIGO Bridges theGap Amaldi-6 -Amaldi-6 Barish 11 Sensitivity of DECIGO 10–18 Laser: 10W, 532nm –19 ] Mass: 100kg 10 LISA Mirror: 1m dia. 1/2 10–20 10–21 10–22 –23 DECIGO 10 (LISA type, 5x104km) Strain [1/Hz –24 10 DECIGO LCGT (FP type, 1000km) 10–25 10–4 10–3 10–2 10–1 100 101 102 103 Frequency [Hz] Force noise= 1/100 of LISA’s 24-June-05 Amaldi-6 - Barish 12 Resonant Bar MiniGrail Auriga, Italy The Netherlands Detectors Allegro USA Schenberg Brazil Nautilus, italy Explorer Switzerland Niobe 24-June-05 Amaldi-6 - Barish Australia 13 24-June-05 Amaldi-6 - Barish 14 “spheres” • omnidirectionality: decode the excitation of the 5 quadrupolar modes to get uniform sky coverage & find direction of propagation • cross section: larger as the volume fill-up factor in respect to bars MiniGRAIL (Leiden-Rome) just started operation Talks of Annette de Waard and Luciano Gottardi Schenberg (Brasil) coming to 24-June-05 Amaldi-6 - Barish 15 DUAL: two nested resonant masses Cerdonio et al PRL (2001), Bryant et al PRD (2003), Bonaldi et al PRD (2003) read-out with non-resonating transducers the differential deformations at frequencies between the lowest quadrupolar modes GW signals add talk by Michele Bignotto back action noises subtract sensitive in a few kHz-wide freq band !!! sensitivities in the 2006 - 2012 prospective 24-June-05 Amaldi-6 - Barish 17 Bar Network 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. 24-June-05 Amaldi-6 - Barish 19 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 ΔE ~ 0.02 M converted @ 10 kpc 24-June-05 [P. Astone, et alAmaldi-6. Phys. - Rev. Barish D68 (2003) 022001] 20 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 Number of events Sidereal hours ROG Coll.: CQG 19, 5449 (2002) L.S.Finn: CQG 20, L37 (2003) P.Astone, G.D’Agostini, S.D’Antonio: CQG Proc. Of GWDAW 2002,New gr-qc/0304096 data E. Coccia ROG Coll.:CQG Proc. Of GWDAW 2002 ROG Coll.: gr-qc/0304004 needed 24-June-05 Amaldi-6 - Barish 21 EXPLORER NAUTILUS Science Run 03 - crewless operation -data validated by cosmic ray effect - new upper limit with bars, no significant coincidence excess nor sidereal effect. ROG S 01 suggestion ROG S 03 24-June-05 Amaldi-6 - Barish 22 IGEC-2 Expected Performance Triple coincidences: 106 time shifts, no accidentals, 9.3 days false alarm rate < 10-4 / yr for H>1.4 10-21/Hz Double coincidences: lower false alarm rates than for IGEC-1 My best guess on the achievable IGEC-1 upper limit upper limit improvement by IGEC-2 1 month dashed region excluded rate with probability [year –1] > 90% WARNING: 1 year incomplete data set ! search threshold 24-June-05 Amaldi-6 - Barish 23 LIGO Louisiana TAMA Japan 4000m 300m Interferometer Detectors Virgo Italy 3000m GEO Germany AIGO Australia 600m future LIGO Washington 2000m & 4000m 24-June-05 Amaldi-6 - Barish 24 TAMA 24-June-05 Amaldi-6Kanda - Barish 25 TAMA 24-June-05 Amaldi-6Kanda - Barish 26 S4 Sensitivity 24-June-05 Amaldi-6 - Barish 27 Noise Progression of the Louisiana Interferometer 24-June-05 Amaldi-6 - Barish 28 Results for Neutron Star Binaries Event Candidates » 142 event candidates found in the data » Loudest candidates eliminated in follow up investigation… » Other candidates consistent with background of analysis pipeline Upper limit set on the rate of BNS coalescences R90 = 47 / year / MWEG 24-June-05 Amaldi-6 - Barish 29 Results for Primordial Black Hole Binaries Same analysis pipeline Event rate consistent with background of analysis pipeline Upper limit set on the rate of PBHB coalescences R90 = 63 / year / MWEG 24-June-05 Amaldi-6 - Barish 30 Stochastic Background Predictions and Experimental Limits LIGO S1, 2 wk data 2 Laser Interferometer Ω h100 < 23 PRD 69(2004)122004 0 0 Space Antenna - LISA (H2-L1) -2 ) LIGO S3, 2 month data 2 Nucleosynthesis2 -4 Ω0h100 < 4.4x10 100 -4 Pulsar h Cosmic strings (H1-L1) presented here 0 Initial LIGO, 1 yr data 2 -6 Expected Ω h100 < 2x10 Ω -6 0 ( (H1-L1)LIGO band -8 Advanced LIGO, 1 yr data Log Pre-big bang 2 -10 CMB Expected Ω0h100 < 7x10 -10 model (H1-L1) EW or SUSY -12 Inflation Phase transition -14 Slow-roll Cyclic model -18 -16 -14 -12 -10 -8 -6 -4 -2 0 2 4 6 8 10 Log ( f [Hz]) f ~ H0 - one oscillation in the f ~ 1/Plank scale – red shifted from lifetime of the universe the Plank era to the present time 24-June-05 Amaldi-6 - Barish 31 Conclusions Sensitivity toward gravitational wave detection is improving on many fronts and this will continue well into the future New upper limits are being set for the major sources -- binary inspirals, periodic sources, burst sources and stochastic background. Data exchange and joint data analysis between detector groups is improving our ability to make detections Many exciting future projects and upgrades are planned or getting underway. Hopefully, detections will be made soon !! Maybe by Amaldi-7?? 24-June-05 Amaldi-6 - Barish 32 THANKS See at Amaldi-6 Amaldi-7 Organizers!!! Sydney 24-June-05 Amaldi-6 - Barish 33.
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