LIGO-G060317-00-Z
QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. GWADW Elba 2006
Auriga, Explorer and Nautilus
Eugenio Coccia INFN Gran Sasso and U. of Rome “Tor Vergata” QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture.
QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture.
QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Frequency emitted by a dynamic system of density ρ :
f ~ Gρ kHz frequencies correspond to nuclear densities (10-15 g/cm3)
Sources: compact objects • gravitational collapse to form neutron star or black hole, • last orbits of an inspiraling neutron star or black hole binary system, its merging, and its final ringdown, • starquakes, phase transitions neutron to quark star EXPERIMENTALEXPERIMENTAL CONFIGURATIONCONFIGURATION
Vp
R p
Cd Antenna M L 0 Li
Capacitive Superconducting dc-SQUID transducer Low-dissipation M = 10 nH Transformer s -6 Al 5056 Φn= 3 ·10 Φo/√Hz Lo=2.86 H mt = 0.75 kg Li=0.8μH νt= 916 Hz K=0.8 Ct = 11 nF E = 2.6 MV/m EXPLORER Duty cycle > 90%
Astone et al.(ROG Collaboration) Phys. Rev. Lett. 2003
The bandwidth depends The peak sensitivity NAUTILUSmainly on the 2004 depends on T/MQ Dutytransducer cycle and > amplifier 90%
T noise = 690 μK AURIGA Status: duty cycle, sensitivity and physics @ T=4.5 K
AURIGA T=4.5K - noise prediction • 1 year of continuous data taking with sensitivity 1x10-19 - mechanical thermal - LC thermal - SQUID back action - SQUID additive -21 -21 -1/2 1.5x10 < Sh< 5x10 Hz within a 100 Hz band •Thorough study of intrinsic noise via fluctuation/ dissipation theorem: small fluctuations agree with 1x10-20 Re{1/Z(ω)} (thermal noise) ]
-1/2 • Detector sensitivity is dominated by thermal noise of bar
[Hz and 2 modes transducer (purple + blu lines) 0.5
hh -21 S 1x10 • Events due large fluctuations in the 800 1000 Hz band mostly due to up-conversion of noise in the very low frequency band (5-70 Hz) but limited to few events per day 1x10-220.23 800 850 900 950 1000 ethr/4.5:on 0.22 × 10 -21 Frequency [Hz] -22 -1 0.21 • Noise rms 1.5 10 Hz (i.e. gw strain noise integrated over the detector bandwidth h ~10-19 ) 0.2 rms • Good noise level stability: rms of noise in the full 0.19 detection bandwidth fluctuates less than 25% 0.18 • Short peaks correpond to 4He refilling (few hours) 0.17 • Each dot represent 3 hours of data taking Sigma [1/Hz] 0.16
0.15
0.14 19/05/05 18/06/05 18/07/05 17/08/05 16/09/05 16/10/05 15/11/05 Time [date] amp*4.5/ethr {amp*4.5/ethr<30}Joint search of gw burst events From IGEC2 events lists of 6 months (May-NovEntries 2005) 187253 10 4 • Duty time 96.6% (after epoch vetoes) 10 3 • 45 events/hour @ 4.5 2 • Few events @ SNR > 6 per day Counts 10 • Only 85 very large events with SNR> 30 10 • Event lists ready for IGEC2 coincidence analysis 1 5 1015202530 Amplitude of a 1ms burst SNR SNR=4.5 → h ~1.4 10 -18 AURIGA targeted searches of gw • Search for periodic signal from binary pulsars with SGR1806-20 giant flare time of Dec 27 2004 em phase measured by Radio Telescopes • Search for gw flux from stationary sources using the Antenna Pattern properties (sidereal time analysis) ε • Search for gw in coincidence with X or Gamma flares emitted by Soft Gamma Repeaters (SGR) e Gamma Ray Bursts (GRB) e.g. the giant flare of SGR1806-20 due to crustal failure of a magnetar (see L. Baggio et al. Phys Rev Lett 95 081103 (2005)) 95%confidence upper limits on gw energy -6 2 emitted @ the flare time:εgw<5 10 MOc Explorer and Nautilus status Explorer at T= 3 K Calibration signal Nautilus at T= 3.5 K 10-17 Since 2003 in continuous data taking with a -22 1/2 -20 sensitivity 8·10 [Hz Analysis of the Explorer-Nautilus 1/2 h S coincidences in the years 2001 and 2003 -20 10 already published, in progress for 2004. 10-21 IGEC2 joint search for GW burst events in 10-22 the period May-December 2005 in progress. 840 880 920 960 1000 f (Hz) Variance of the noise computed over 10 minutes before each event in the period May-December 2005 10 6 10 6 Nautilus Explorer 10 5 10 5 Counts Counts 10 4 10 4 10 3 10 3 10 2 10 2 1 10 1 10 0 10 0 10 -22 -21 -21 -21 -21 -21 0 5 10 -22 1 10 -21 1,5 10 -21 2 10 -21 2,5 10 -21 3 10 -21 0 5 10 1 10 1,5 10 2 10 2,5 10 3 10 sigma [Hz -1 ] sigma [Hz -1 ] www.lnf.infn.it/esperimenti/rog Distribution of the SNR of the events in the period May-December 2005, for IGEC2 coincidence analysis 106 106 Nautilus Explorer 105 105 4 4 Counts 10 Counts 10 103 103 102 102 101 101 100 100 0 5 10 15 20 25 30 0 5 10 15 20 25 30 SNR SNR • Operation with high duty cycle. In the period May-December 2005: Explorer 89%, Nautilus 90% (preliminary - validation in progress). •99% of events associated to a noise with sigma < 6.9 10-22 Hz-1(Explorer) and < 4.7 10 -22 Hz-1 (Nautilus) Cumulative analysis of the association between the data of the gravitational wave detectors NAUTILUS and EXPLORER and the gamma ray bursts detected by BATSE and BeppoSAX Phys. Rev. D 71, 042001 (2005) www.lnf.infn.it/esperimenti/rog NAUTILUSNAUTILUS OPERATIONSOPERATIONS DURINGDURING AprilApril 20020055 Duty Cycle ∼ 85 % Liquid Helium Refillings Days of April 2005 IGEC 2 The IGEC Network of 4 Resonant Detectors set upper limits for burst signals The EXPLORER/NAUTILUS SEARCH FOR SHORT GW BURSTS 1997- 2000 IGEC search PRL 85, 5046 (2000) 1998 931 hours; CQG 18, 43 (2001) 2001 2156 hours; CQG 19, 5449 (2002) 2003 3677 hours; CQG Amaldi 6, (2006) 2004 5196 hours; Analysis being completed 2005 Analysis in progress in the IGEC2 framework T 2001 2003 2004 DIRECTIONALITYDIRECTIONALITY INTERFEROMETER BAR DETECTOR 6 4 1998 2 0 4 2001 2 0 4 2003 2 0 G. Paturel, Yu.V. Barishev Sidereal time analysis as a tool for study of the space distribution of gw sources. Astro-ph/0211604v1, A&A 398, 377 (2003) The expected rate of events on EXPLORER for sources on the galactic disc and on the GC *= coincidences ______= accidentals gr-qc 0405047, PRD 2004 gr-qc 0405145 Cosmic ray Excitation of the longitudinal modes interaction in the bar of a cylindrical bar Thermo-Acoustic Model: the energy deposited by the particle is converted in a local heating of the medium: A resonant gw detector used as a particle detector is different from any other particle detector δE δT = ρCV0 δE αY δp = γ γ = V0 ρC γ = Gruneisen “constant” Effect of cosmic rays EXPLORER is equipped with 3 NAUTILUS is equipped with 7 layers layers (2 above the cryostat - area (3 above the cryostat - area 36m2/each 13m2 - and 1 below -area 6 m2) - and 4 below -area 16.5 m2/each) of of Plastic Scintillators. Streamer tubes. The cosmic ray effect on the bar is measured by an offline correlation, driven by the arrival time of the cosmic rays, between the observed multiplicity in the CR detector (saturation for M≥103 particles/m2) and the data of the antenna, sampled each 4.54 ms and processed by a filter matched to δ signals ΔE = 1 mK = 0.15 μeV Explorer ev/giorno tutto 2003 predizioni EXPLORER 2002 >600 P M2 Nautilus 2003 ev giorno Nautilus 2000-2001 ev/giorno Ev/Giorno Nautilus 98 Nautilus 2000 T<1 K 100 Sommario dati coincidenze 10 raggi cosmici 1998 ad oggi 1 predizioni 0.1 0.01 Ev/Giorno Distribuzione integrale Ev/Giorno Distribuzione 0.001 0.001 0.01 0.1 1 10 Sqrt(kelvin) 10-18 2006-2007 Network h/ĆHz 2006 - 2007 Network LIGO 10-19 Virgo Resonant -20 10 Pulsars Antennas 2007 h , 1 year integration max BH-BH Merger GEO Oscillations @ 100 Mpc -21 10 Core Collapse QNM from BH Collisions, @ 10 Mpc QNM from BH Collisions, 100 - 10 Msun, 150 Mpc 1000 - 100 Msun, z=1 BH-BH Inspiral, 100 Mpc 10-22 NS-NS Merger Oscillations BH-BH Inspiral, @ 100 Mpc z = 0.4 -6 10-23 NS, ε=10 , 10 kpc NS-NS Inspiral, 300 Mpc 10-24 1 10 100 1000 104 Hz Interferometric NS-NS NS-BH BH-BH SNe Network Event Rate (per year) 3 10-4 - 0.3 4 10-4 - 0.5 10-3 - 3 0.05 Range (Mpc) 30 60 145 0.1 10-19 h/ĆHz LIGO+ 2008 -2008-2012 2012 Network Network 10-20 SFERA (Quantum Limit) Pulsars BH-BH Merger Oscillations DUAL Demonstrator h , 1 year integration @ 100 Mpc max (200 hbar, starting 2011) 10-21 QNM from BH Collisions, Virgo+ 100 - 10 Msun, 150 Mpc BH-BH Inspiral, 100 Mpc Core Collapse @ 10 Mpc 10-22 QNM from BH Collisions, 1000 - 100 Msun, z=1 BH-BH Inspiral, NS-NS Merger z = 0.4 Oscillations @ 100 Mpc NS, ε=10-6, 10 kpc -23 10 GEO HF NS-NS Inspiral, 300 Mpc starting 2009/2010 10-24 10 100 1000 Hz 104 Interferometric NS-NS NS-BH BH-BH SNe Network Event Rate (per year) 0.025-10 10-3-15 3 10-2-90 1 Range (Mpc) 114 230 584 10 www.minigrail.nl Sensitivity predicted for next run 3 x 10-22 Dual Main Concept -gwsignals add - - back action noises subtract - MC et al. PRL 87 (2001) 031101 MB et al. PRD 68 (2003) 102004 The outer The inner resonator is π Phase resonator is Read the differential driven above difference driven below deformations of two resonance frequency nested resonators 3-5 kHz Intermediate GW broadband Spectral sensitivity @ SQL Mo Dual 16.4 ton height 2.3m 0.94m SiC Dual 62.2 ton height 3.0m 2.9m Q/T=2x108 K-1 Antenna pattern: like 2 IFOs co- M. Bonaldi et al. located and rotated by 45° Phys. Rev. D 68 102004 (2003) M. Bonaldi et al. gr-qc/0605004 Conclusions • Auriga, Explorer and Nautilus are taking data continuously with high duty cycle • Events lists of 6 months May-Nov 2005 ready for analysis • Explorer-Nautilus coincidence search 1998-2004 published soon: excitements and limits of a two-detectors coincidence search. • INFN Roadmap: Bars ON up to 2009. No large Spherical detector project. Continuation of the R&D for Dual.