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lecture - Ettore Majorana - Infn

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“<strong>Ettore</strong> <strong>Majorana</strong>” Foundation and Centre for Scientific CultureInternational School of Subnuclear Physics – Erice June 30, 2012Gravitational Wavesand High Energy PhysicsEugenio CocciaU. of Rome “Tor Vergata” and INFNChair of the Gravitational Wave International Committee


Gravity is a manifestation of spacetime curvature induced by mass-energy 10 non linear equations in the unknown g µνcomponents of the metric tensords 2 =g µν dx µ dx ν spacetime tells matter how to move; matter tells spacetime how to curve


PSR1913+16: GWs do exist • Pulsar bound to a “dark companion”, 7 kpcfrom Earth.• Relativistic clock: v max /c ∼10-3 • GR predicts such a system to loose energy viaGW emission: orbital period decreases • Radiative prediction of general relativityverified at 0.2% level P (s) dP/dt dω/dt (º/yr) M p M c 27906.9807807(9) -2.425(10)·10 -12 4.226628(18) 1.442 ± 0.003 M 1.386 ± 0.003 M Nobel Prize 1993: Hulse and Taylor


• No laboratory equivalent of Hertz experiments for production of GWsLuminosity due to a mass M and size R oscillating at frequency ω~ v/R:L = 2G5c 5Q ˙ ˙ 2 ≈ GM2 v 6R 2 c 5M=1000 tons, steel rotor, f = 4 Hz L = 10 -30 WEinstein: “ .. a pratically vanishing value…”Q ≈ MR 2 sinωtCollapse to neutron star 1.4 M oL = 10 52 Wh ~ L 1/2 d -1 ; source in the Galaxy h ~ 10 -18 , in VIRGO cluster h ~ 10 -21Fairbank: “ ...a challenge for contemporary experimental physics..”


Gravitational radiation is a tool for astronomical observationsGWs can reveal features of their sources that cannot be learnt byelectromagnetic, cosmic rays or neutrino studies (Kip Thorne)- GWs are emitted by coherent acceleration of large portion of matter- GWs cannot be shielded and arrive to the detector in pristine condition


GW amplitude due to the isotropic conversionof a mass M in GWsh = 2 ⋅10 −19$&%8kpcr')(M GW10 −4 M •


• GWs are detectable in principleThe equation for geodetic deviation is the basis for all experimental attempts todetect GWs:d 2 δl jdt 2 = −R jokol k = 1 2∂ 2 h jk∂t 2• GWs change (δl) the distance (l) between freely-moving particles in emptyspace.They change the proper time taken by light to pass to and fro fixed points inspaceIn a system of particles linked by non gravitational (ex.: elastic) forces, GWsperform work and deposit energy in the systeml kLh = ΔLL˙ x (t) + τ −1˙ x (t) +ω 2 0x(t) = l h ˙ (t)2LBeam splitterPhoto detectorImpossibile visualizzare l'immagine. La memoria del computer potrebbe essere insufficiente per aprire l'immagine oppure l'immagine potrebbeessere danneggiata. Riavviare il computer e aprire di nuovo il file. Se viene visualizzata di nuovo la x rossa, potrebbe essere necessario eliminarel'immagine e inserirla di nuovo.


SUPERNOVAE. If the collapse core is non-symmetrical,the event can give off considerableradiation in a millisecond timescale. Information Inner detailed dynamics of supernova See NS and BH being formed Nuclear physics at high density SPINNING NEUTRON STARS.Pulsars are rapidly spinning neutronstars. If they have an irregular shape,they give off a signal at constantfrequency (prec./Dpl.)InformationNeutron star locations near the EarthNeutron star PhysicsPulsar evolution COALESCING BINARIES. Two compact objects (NS or BH) spiraling together from a binary orbitgive a chirp signal, whose shapeidentifies the masses and the distanceSTOCHASTIC BACKGROUND. Random background, relic of the earlyuniverse and depending on unknownparticle physics. It will look like noise in any one detector, but two detectorswill be correlated.InformationMasses of the objectsBH identificationDistance to the systemHubble constantTest of strong‐field general relativity InformationConfirmation of Big Bang, and inflationUnique probe to the Planck epochExistence of cosmic strings


Coupling constants strong e.m. weak gravity0.1 1/137 10 -5 10 -39GW emission: very energetic events but almost no interaction• In SN collapse ν withstand 10 3 interactions beforeleaving the star, GW leave the core undisturbed • Decoupling after Big Bang– GW ∼ 10 -43 s (T ∼ 10 19 GeV) – ν ∼ 1 s (T ∼ 1 MeV) – γ ∼ 10 12 s (T ∼ 0.2 eV) Ideal information carrier,Universe transparent to GW all the way back to the Big Bang!


Relic Stochastic Background Relic gravitonsRelic neutrinosCMBR• Imprinting of the early expansion of the universe • Correlation of at least two detectors needed


GW OBJECTIVESFIRST DETECTIONtest Einstein prediction8πGcG =4TASTRONOMY & ASTROPHYSICSlook beyond the visible,understand Black Holes,Neutron Stars and supernovaeunderstand GRBCOSMOLOGYthe Planck time:look as back in time as theorist can conceive


Every newly opened astronomical window has found unexpected results


The search for gravitational waves f λ method sources10 -16 Hz 10 9 ly Anisotropy of CBR - Primordial10 -9 Hz 10 ly Timing of ms pulsars - Primordial- Cosmic strings10 -4 - 10 -1Hz0.01 - 10AUDoppler Tracking ofspacecraftLaser interferometersin space LISA- Bynary stars- Supermassive BH (10 3 -10 7 M o )formation, coalescence, inspiral10 - 10 3 Hz 300 - 30000kmLaser interferometerson EarthLIGO, VIRGO, GEO,TAMA- Inspiral of NS and BH binaries(1-1000 M o )- Supernovae- Pulsars10 3 Hz 300 km Cryogenic resonantdetectorsALLEGRO, AURIGA,EXPLORER, NAUTILUS- NS and BH binary coalescence- Supernovae- ms pulsars


Allegro, USAMiniGRAILThe NetherlandsAuriga,ItalySchenberg,BrazilExplorerSwitzerlandNautilus, ItalyNiobeAustralia


THE INTERFEROMETER NETWORK LIGO – Hanford, WA A network of 4 (5) GW detectors GEO600, Hannover, Germany LIGO – Livingston, LA VIRGO, Cascina (PI), Italy BUILDING UP A “SINGLE MACHINE” Virgo and LSC (LIGO ScienEfic CollaboraEon)* have signed an MoU for full data sharing and common authorship of science papers. *GEO600 part of the LSC


GW hunters are heirsto several great traditions:- high precision mechanical experiments (Cavendish, Eotvos, Dicke..)detection of weak forces applied on mechanical test bodies- precision optical measurements (Michelson, laser developers…)- operation of ultraprecise measurement systems (microwavepioneers of World War II, Weber)- very low temperature physics (Onnes, BCS, Josephson)superfluids and superconductors technology


Some perspective: 40 years of attempts at detection:Since the pioneering work of JosephWeber in the ‘70, the search forGravitational Waves has never stopped,with an increasing effort of manpowerand ingenuity:70’: Joe Weberpioneering work90’ : Cryogenic Bars2005 - : Large InterferometricDetectors20


NAUTILUS LNF -­‐ FRASCATI Bar Al 5056 M = 2270 kg L = 2.91 m ; Ø = 0.6 m ν A =935Hz; T = 0.1 K; T = 3 K Readout: Low gap transducer + dc SQUID Cosmic ray detector NAUTILUS gets 4 records: . First ultralow T massive detector: 2.3 tons at 0.09 K. . First acousEc detector of cosmic rays. . Best displacement sensiEvity: 7 x 10 -­‐22 m/Hz -­‐1/2 . Longest GW science run: 10 years (in 2012).


MAIN FEATURESThermal noiseS F = MkTω r /Q V pR pElectronic noiseV n ; I n T n =√V n2 I n2/kAntennaMC dL 0L iThe mechanicaloscillatorMass MSpeed of sound v sTemperature TQuality factor QRes. frequency f rThe transducerEfficiency βThe amplifierNoise temperature T n


Liquid Helium RefillingsTnoise (K)3 mKDays of June 2004For ~ 80% of time the sensitivity to short gw bursts is better than h=2.1 * 10 -19


12 hours of typical data


ALLEGRO (LSU) - AURIGA (LNL) – EXPLORER (CERN) – NAUTILUS (LNF)• Published on Phys. Rev. D82 022003, 2010 .http://arxiv1.library.cornell.edu/abs/1002.3515v1• 515 days of observation. from 16 November 2005 to 14 Aprile 2007. Search forcoincidences. No coincidences with a background of 1 event / century• in spite of the lower sensitivity respect to interferometers, the “IGEC” limit to thepresence of big GW bursts (h rss >10 -19 Hz -1/2 ) is better of a factor of 2.Complete coverage


09 10Results published on CQG or PRD98AuNa09 10 11 1210 years of science run


EXPLORER-NAUTILUS 2001 data analysisROG Coll.: CQG 19, 5449 (2002)Number of eventsSidereal hoursComments, analysis and studiesL.S.Finn: CQG 20, L37 (2003)P.Astone, G.D’Agostini, S.D’Antonio: CQG 20, S769 (2003)ROG Coll.:CQG 20, S785 (2003)E.Coccia, F. Dubath, M. Maggiore: PRD 70, 084010 (2004)


Cosmic rayinteraction in the barThermo-Acoustic Model:the energy deposited bythe particle is converted in alocal heating of themedium:Excitation of the longitudinal modesof a cylindrical barA resonant gw detector used as aparticle detector is different fromany other particle detectorδp = γ δEV 0δT =δEρCV 0γ = αYρCγ = Gruneisen “constant”


Effect of cosmic raysEXPLORER is equipped with 3layers (2 above the cryostat - area13m 2 - and 1 below -area 6 m 2 )of Plastic Scintillators.NAUTILUS is equipped with 7 layers(3 above the cryostat - area 36m 2 /each- and 4 below -area 16.5 m 2 /each) ofStreamer 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 observedmultiplicity in the CR detector (saturation for M≥10 3 particles/m 2 ) and thedata of the antenna, sampled each 4.54 ms and processed by a filtermatched to δ signalsΔE = 1 mK = 0.15 µeV


Nautilus as acoustic particle detectorInteraction of a particle with a bar: ionizationenergy lost is converted in thermal heating andtherefore pressure wave. The detectionmechanism is quite simple, no threshold in β“calorimetric measurement” Nautilus is able to detect energy releasesas low as 10 -7 eV (10 -26 J) by measuringthe excitation of the longitudinal mode ofVibration.Nautilus is equipped with streamer tubesparticle detectorsCosmic rays: observedExotic form of matter: observableUpper limit for nuclearite flux from the Rome GWresonant detectorsPhys.Rev. D47:4770-4773, 1993Cosmic rays observed by NAUTILUSPhys.Rev.Lett. 84:14-17, 2000.Detection of high energy cosmic rays with NAUTILUSAstropart.Phys. 30:200-208, 2008.


Detectable signals todayBURSTS: Black Hole (M~10Mo) formation, 10-4Mo into GWSNR = 6 ×10 3 " 10kpc$2 " 10 −44 Hz −1 $'# r % # h ˜ 2 (" Δf $%#1Hz%SPINNING NEUTRON STARS: Non axisymmetric (ε~10-6)pulsar, M~1.4Mo"SNR ≈ 30 10kpc $2 " 10 −44 Hz −1 $ " ε $ " T'# r % # h ˜ 2 (obs$%#10 −6 ' (%#1y %COALESCING BINARIES: Inspiraling NS-NS system,M~1.4MoSNR ≈ 10 3 " 10kpc$2 " 10 −44 Hz −1 $'# r % # h ˜ 2 (" Δf $%#1Hz%STOCHASTIC BACKGROUND: 2 detectors, at distanced


Exploiting the resonant-mass detector technique:the spherical detector • 5 quadrupole modes• Source direction• Wave polarizationM = 1-100 tonsSensitivity:10 -23 - 10 -24 Hz -1/2 ;h ~ 10 -21 - 10 -22• 3 kHz spheresMiniGrail (Leiden, NL)Sfera (Frascati, I)Shenberg (Sao Paulo, B)


The phase change and the future1960 - 2005Given the uncharted territory that gravitational-wave detectorsare probing, unexpected sources may actually provide the firstdetection.2005 -Only new high sensitivity detectors can provide the firstdetection and open the GW astronomyThe contribution of Resonant Bars has beenessential in establishing the field, givinginteresting results and putting someimportant upper limits on the gravitationallandscape around us, but now the hope forguaranteed detection is in the Network oflong arm interferometers.34


LAPP - AnnecyINFN - Firenze/UrbinoIPN - LyonINFN - NapoliOCA - NiceNikhef - AmsterdamESPCI - ParisLAL - OrsayINFN - PerugiaINFN - PisaINFN – RomaINFN - Roma Tor VergataInaugurated July 2003


Principle of operationInterferometers use laser light tocompare the lengths of twoperpendicular armsh =(L + ΔL) − (L − ΔL)L= 2 ΔLLLWhen the wave arrives, the twoarms respond differently, they areno longer the same length, andso the two beams are no longerin phase, producing a shift in theinterference fringes. LBeam splitterPhoto detector


Vacuum: 10 -9 mbarA real detector scheme Isolation fromground vibrations3-4 km long Fabry-Perotcavities: lengthen theoptical path to 100 km10-20 W LaserPower recycling mirror:increase the light powerto 1 kWlarge fused silica mirrors(low thermal noise)Input optics


Limits to SensitivityVibrational Noise!• Groundmotion!• Acoustic!Residual Gas Noise!!Thermal Noise!• Test masses!• Suspensions!• Coatings!Laser Noise!• FrequencyNoise!• Intensity Noise!Quantum Noise!• Shot Noise!• RadiationpressureNoise!LIGO-G1101272-v1 ICGC, Goa"39"


Virgo "• Virgo"– European collaboration, located near Pisa"– Single 3 km interferometer, similar to LIGO in design andspecification"– Advanced seismic isolation system (“Super-attenuator”)"• Advanced Virgo"– Similar in scope and schedule to Advanced LIGO"• Joint observations with LIGO since May 2007"


Virgo - Main requirements!• Vacuum!Base pressure (H 2 ) ! ! !10 -9 mbar!Hydrocarbons ! ! ! !10 -14 mbar!• Seismic attenuation ! ! 10 11 at 10 Hz!• Nd-YAG Laser (at 1kHz)!frequency ! ! ! ! 10 -6 Hz 1/2 !power ! ! ! ! ! 3x10 -7 Hz -1/2 !beam jitter ! ! ! ! 10 -10 rad Hz -1/2 !• Mirrors!Substrate losses and coating losses ! !ppm!Surface deformation ! ! !λ/100 (0.01µm)!• Data flow ! ! ! !4 Mbyte/s!


Seismic noisereduction:Superattenuators• Need !10 11 attenuation @ 10 Hz!27


"• GEO Collaboration"GEO "– GEO as a whole is a member of the LIGO ScientificCollaboration"– GEO making a capital contribution to Advanced LIGO "• GEO600"– Near Hannover"– 600 m arms"– Signal recycling"– Fused silica suspensions"• GEO-HF"– Up-grade underway"– Pioneer advanced optical techniques "48"


LSC and Virgo recent papersDirectional limits on persistent gravitational waves using LIGO S5 science data.Phys. Rev. Lett. 107:271102, 2011.Beating the spin-down limit on gravitational wave emission from the Vela pulsar.Astrophys. J. 737, 93, 2011Search for Gravitational Wave Bursts from Six Magnetars.Astrophys. J. 734, L35, 2011Search for gravitational waves from binary black hole inspiral, merger and ringdown.Phys. Rev. D83:122005, 2011Search for GW inspiral signals associated with Gamma-Ray bursts during LIGO's fifth and Virgo's first science run.Astrophys. J. 715:1453-1461, 2010.Searches for gravitational waves from known pulsars with S5 LIGO data.Astrophys. J. 713:671-685, 2010.Search for GW bursts associated with Gamma-Ray bursts using data from LIGO Science Run 5 and Virgo Science Run 1.The LIGO and the Virgo CollaborationsAstrophys. J. 715:1438-1452, 2010.All-sky search for gravitational-wave bursts in the first joint LIGO-GEO-Virgo run.Phys. Rev. D81, 102001, 2010Search for Gravitational Waves from Compact Binary Coalescence in LIGO and Virgo Data from S5 and VSR1.Phys. Rev. D82, 102001, 2010An upper limit on the stochastic GW background of cosmological originNature 460, 08278, 2009


Virgo!Results from Initial Detectors:Some highlights from LIGO and Virgo"Several ~year long science data runs by LIGO and VirgoSince 2007 all data analyzed jointly • Limits on GW emission from known msec pulsars – Crab pulsar emitting less than 2% of available spin-down energy ingravitational waves • Limits on compact binary (NS-NS, NS-BH, BH-BH) coalescence rates inour local neighborhood (~20 Mpc) • Limits on stochastic background in 100 Hz range – Limit beats the limit derived from Big Bang nucleosynthesis


1st GENERATIONDETECTORS 1 ST GENERATION INTERFEROMETERS CAN DETECT A NS-­‐NS COALESCENCE AS FAR AS VIRGO CLUSTER (15 MPc) BUT THE EVENT RATE IS TOO LOW !! EXPECTED EVENT RATE: 0.01-­‐0.1 ev/yr (NS-­‐NS) FIRST DETECTION: POSSIBLE BUT UNLIKELY


FROM DISCOVERY TO ASTRONOMY 2 nd generaBon detectors: Advanced Virgo, Advanced LIGO Enhanced LIGO/Virgo+ 2009 Virgo/LIGO GOAL: sensiEvity 10x bejer à look 10x further à DetecBon rate 1000x larger 10 8 ly NS-­‐NS detectable as far as 300 Mpc BH-­‐BH detectable at cosmological distances 10s to 100s of events/year expected! Adv. Virgo/Adv. LIGO 2014 Credit: R.Powell, B.Berger


A Global Array of GWDetectors"LIGOGEOVirgoLCGT• Detection confidence• Locate sources• Decompose thepolarization ofgravitational waves54"


Large Cryogenic GravitaBonal-­‐wave Telescope LIGO-G1101272-v1 ICGC, Goa55


• Project approved July 2010"Large Cryogenic Gravitational-waveTelescope (LCGT)"• LCGT Project"– Lead institution: Institute for Cosmic Ray Research"– Other participants include University of Tokyo, NationalAstronomical Observatory of Japan, KEK, …"• Key Design Parameters"– Underground (Kamioka mine)"– Sapphire test masses cooled to


Completing the Global Network"LIGOGEOVirgoLCGTLIGO-IndiaPlanned detectorsare very close toco-planar—notoptimal for all-skycoverage!! ! Large increase toscience capabilityfrom a southernnode in the network!


Localization capability:LIGO-Virgo only"58"


Localization capability:LIGO-Virgo plus LIGO-India"


LIGO-India Concept"• A direct partnership between LIGO Laboratory and IndIGOcollaboration to build an Indian interferometer"– LIGO Lab (with its UK, German and Australian partners)provides components for one Advanced LIGO interferometerfrom the Advanced LIGO project"– India provides the infrastructure (site, roads, building,vacuum system), “shipping & handling,” staff, installation &commissioning, operating costs"• LIGO-India would be operated as part of LIGO network tomaximize scientific impact"


Sensitivity curvesh (Hz -1/2 )1010-19Pulsarsh max – 1 yr integrationLIGO1 st generation detectorsCredit: P.Rapagnani10-2010-2110-22VirgoQNM from BH Collisions,1000 - 100 Msun, z=1BH-BH Inspiral,z = 0.4-181 10 100 1000 10 4GEOQNM from BH Collisions,100 - 10 Msun, 150 MpcBH-BH Inspiral, 100 MpcBH-BH MergerOscillations@ 100 MpcResonantantennasCore Collapse@ 10 MpcNS-NS MergerOscillations@ 100 Mpc10-23NS, ε =10 -6 , 10 kpcNS-NS Inspiral, 300 Mpc10-24Hz


AURIGA - LNLNAUTILUS - LNFData AUNA Taking We are here´06 ´07 ´08 ´09 ´10 ´11 ´12 ´13 ´14 ´15 ´16 ´17 ´18 ´19 ´20 ´21 ´22VirgoGEOLIGOLISAHanfordLivingstonVirgo+LIGO+Advanced VirgoGEO HFAdvanced LIGOLaunch Transfer dataE.T.DS PCP Construction CommissioningdataWindow of opportunityfor AURIGA and NAUTILUS62


exercise in recovering injected gw signals of 8•10 -5 M solar total energywith coherent wavebursts analysis (G.Vedovato for AUNA)Sn explosions according to the acoustic model s25.0; chirps ofrandom polarization randomly injected in the Galaxy accordingly tothe star density; injections over 1day of AUNA datadetection efficiency vsdistanceDistribution in the Galactic planeof the injections (colour) and ofthe recovered signals (black)


Newtonian Gravitational NoiseBARS!!/ VIRGO!SPHERES!


Third Generation Science


TestMassesTelescopesSpacecrafts5 10 6 km3 pairs of “free falling” testmasses( 3 10 -15 ms -2 Hz -1/2 @ 0.1 mHz)3 “test-mass follower”shielding spacecraft2 semi-independent 5 10 6 kmMichelson Interferometerswith Laser Transponders( 40 pm Hz -1/2 )Goal: GW at0.1 mHz – 0.1 HzSensitivity4 10 -21 Hz -1/2 @ 1 mHz


• Savings mainly in weight, launch cost.• Two active arms, not three;• Smaller arms (1Gm, not 5Gm);• Re-use LISA Pathfinder hardware;


More about GW and HEP


Millisecond pulsars are rapidly rotating, highlymagnetized neutron stars which emit a beam of electromagneticradiation that sweeps over the Earth once perrotation.They constitute extremely accurate clocks thatcould be used to detect GWs. Candidates for the generationof a GW background in the nano-Hz band are supermassiveblack hole binary mergers and cosmic strings .


Another potential candidate for these detectors:The cosmological QCD phase transition, which is believed tohave taken place when the Universe had a temperature ofT = 100 MeV. A GW background can be generated by theQCD phase transition if it is first order, and the characteristicfrequency of this background falls in the frequencyband of pulsar timing experiments.If the phase transition is sufficiently strong and lasts for asufficiently long time, the GWs produced can be observedin future pulsar timing experiments.E. Witten, Phys. Rev. D 30, 272 (1984).


Michele Maggiore, Science (2000) Volume: 331, Issue: May, Pages: 283-367


GRAVITATIONAL WAVES MEET NEUTRINOS:PREPARING FOR THE NEXT NEARBY SUPERNOVACore-collapse supernovae are potential sources of gravitationalwaves and have well established neutrino and optical signatures.The neutrino signal arrives at the observer frame essentiallysimultaneously with the gravitational-wave signal while theobserved optical signal rises within hours after these promptsignals.This sequence of events constitutes the cornerstone of thedetection process in gravitational-wave and neutrino observationsof stellar collapse.


A combined gravitational-wave andneutrino detector network providesbenefits in sensitivity, coincidencelive-time coverage and confidence ofdetection. These arise primarily fromthe tight window of coincidenceexpected for the two signatures.Gravitational waves and neutrinos from core-collapse supernovae areemitted in the inner-most, high density region of the supernova corewhich cannot be probed electromagnetically. Gravitational waves andneutrinos thus become the only messengers that can carry “live”dynamical information from deep inside a dying massive star andconstrain the detailed, yet unknown, mechanism driving the corecollapsesupernova explosion.


Moreover, we can use gravitational waves and neutrinos to identifycore-collapse events that do not lead to a strong electromagneticdisplay. This scenario may occur through the extinction of thesupernova light by intervening material, and/or through “failingsupernovae” in which no, or only a very weak, explosion occursand which may be the birth sites of stellar-mass black holes. Aneutrino and gravitational-wave coincidence, in the absence of anoptical signal, would provide smoking-gun evidence for this scenario.It is worth noting that the rate of such failed supernovae may becomparable to the rate of supernovae with optical signals.C. S. Kochanek, J. F. Beacom, M. D. Kistler, J. L. Prieto, K. Z. Stanek, T. A.Thompson, H. Y¨uksel, 2008, Astrophys. J., 684, 1336.


Goal: implementing a collaborative effort and a real-timecoincidence search, involving all instruments.Aim: primarily, search for events near the threshold of detection inboth the neutrino and gravitational-wave sectors.Also, it is expected to play a role in the event of a galacticsupernova reported by SNEWS, i.e., for an event cleanly standingout from the analysis in the neutrino detector network alone


Conclusion


THE QUEST FOR GW: OBJECTIVESFIRST DETECTION test Einstein predicEon 8πGcG =4TASTRONOMY & ASTROPHYSICS look beyond the visible understand BH, NS and supernovae understand GRB COSMOLOGY the Planck Eme: look as back in Eme as theorist can conceive


• We are on the threshold of a new era of gravitational waveastrophysics"• First generation detectors have broken new ground in opticalsensitivity"– Initial detectors have proven technique"• Second generation detectors are starting installation"– Will expand the “Science” (astrophysics) by factor of 1000"• In the next decade, emphasis will be on the NETWORK "


http://gwic.ligo.org/index.shtml


VisibleInfraredCOBEγ-rayThere are more things in the heavenand in earth, Horatio, than are dreamtof in your philosophy[Hamlet I.5]GRBsGWs ???


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