Probing the Universe for Gravitational Waves
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1 Probing the Universe for Gravitational Waves Barry C. Barish Caltech Crab Pulsar Georgia Tech 26-April-06
2 General Relativity the essential idea G μν = 8πΤ μν Gravity is not a force, but a property of space Overthrew & time Objects Concentrations follow the the 19 of th shortest mass -century or path energy concepts through distort of» this absolute Spacetime = 3 spatial and time dimensions + time (warp) warped spacetime spacetime; path is the same for» all Perception objects of space or time is relative 26-April-06 LIGO - Georgia Tech 2
3 After several hundred years, a small crack in Newton s theory.. perihelion shifts forward an extra +43 /century compared to Newton s theory 26-April-06 LIGO - Georgia Tech 3
4 A new prediction of Einstein s theory Light from distant stars are bent as they graze the Sun. The exact amount is predicted by Einstein's theory. 26-April-06 LIGO - Georgia Tech 4
5 Confirming Einstein. bending of light A massive object shifts apparent position of a star Observation made during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster 26-April-06 LIGO - Georgia Tech 5
6 A Conceptual Problem is solved! Newton s Theory instantaneous action at a distance Einstein s Theory information carried by gravitational radiation at the speed of light 26-April-06 LIGO - Georgia Tech 6
7 Einstein s Theory of Gravitation Gravitational waves are necessary consequence of Special Relativity with its finite speed for information transfer Gravitational waves come from the acceleration of masses and propagate away from their sources as a space-time warpage at the speed of light gravitational radiation binary inspiral of compact objects 26-April-06 LIGO - Georgia Tech 7
8 Einstein s Theory of Gravitation gravitational waves Using Minkowski metric, the information about space-time curvature is contained in the metric as an added term, h μν. In the weak field limit, the equation can be described with linear equations. If the choice of gauge is the transverse traceless gauge the formulation becomes a familiar wave equation 1 c t 2 2 ( 2 2 ) h μν = 0 The strain h μν takes the form of a plane wave propagating at the speed of light (c). Since gravity is spin 2, the waves have two components, but rotated by 45 0 instead of 90 0 from each other. h h ( t z / c) + hx ( t z / c) = + 26-April-06 LIGO - Georgia Tech 8 μν
9 The Evidence T h e For Gravitational Waves Russel A. Hulse Source: Discovered and Studied Pulsar System PSR with Radio Telescope Joseph H.Taylor Jr 26-April-06 LIGO - Georgia Tech 9
10 The evidence for gravitational waves Hulse & Taylor 17 / sec Neutron binary system separation = 10 6 miles m 1 = 1.4m m 2 = 1.36m e = period ~ 8 hr Prediction from general relativity PSR Timing of pulsars spiral in by 3 mm/orbit rate of change orbital period 26-April-06 LIGO - Georgia Tech 10
11 Indirect evidence for gravitational waves 26-April-06 LIGO - Georgia Tech 11
12 Direct Detection Gravitational Wave Astrophysical Source Detectors in space LISA Terrestrial detectors LIGO, TAMA, Virgo, AIGO 26-April-06 LIGO - Georgia Tech 12
13 Gravitational Waves in Space LISA Three spacecraft, each with a Y-shaped payload, form an equilateral triangle with sides 5 million km in length. 26-April-06 LIGO - Georgia Tech 13
14 Network of Interferometers LIGO GEO Virgo TAMA decompose detection locate the the confidence polarization sources of gravitational waves AIGO 26-April-06 LIGO - Georgia Tech 14
15 The frequency range of astronomy EM waves studied over ~16 orders of magnitude» Ultra Low Frequency radio waves to high energy gamma rays 26-April-06 LIGO - Georgia Tech 15
16 Frequencies of Gravitational Waves The diagram shows the sensitivity bands for LISA and LIGO 26-April-06 LIGO - Georgia Tech 16
17 Gravitational Wave Detection free masses h = strain amplitude of grav. waves h = ΔL/L ~ L = 4 km ΔL ~ m Laser Interferometer laser 26-April-06 LIGO - Georgia Tech 17
18 Interferometer optical vacuum layout suspended, seismically isolated test masses mode cleaner 4 km laser various optics 10 W 6-7 W 4-5 W W 9-12 kw 200 mw photodetector GW channel 26-April-06 LIGO - Georgia Tech 18
19 Hanford Observatory LIGO Laser Interferometer Gravitational-wave Observatory MIT Caltech Livingston Observatory 26-April-06 LIGO - Georgia Tech 19
20 LIGO Livingston, Louisiana 4 km 26-April-06 LIGO - Georgia Tech 20
21 LIGO Hanford Washington 4 km 2 km 26-April-06 LIGO - Georgia Tech 21
22 LIGO Beam Tube Minimal enclosure Reinforced concrete No services 1.2 m diameter - 3mm stainless 50 km of weld 65 ft spiral welded sections Girth welded in portable clean room in the field 26-April-06 LIGO - Georgia Tech 22
23 Vacuum Chambers vibration isolation systems» Reduce in-band seismic motion by 4-6 orders of magnitude» Compensate for microseism at 0.15 Hz by a factor of ten» Compensate (partially) for Earth tides 26-April-06 LIGO - Georgia Tech 23
24 LIGO vacuum equipment 26-April-06 LIGO - Georgia Tech 24
25 Seismic Isolation suspension system Suspension assembly for a core optic Support structure is welded tubular stainless steel Suspension wire is 0.31 mm diameter steel music wire Fundamental violin mode frequency of 340 Hz 26-April-06 LIGO - Georgia Tech 25
26 LIGO Optics fused silica Surface uniformity < 1 nm rms Scatter < 50 ppm Absorption < 2 ppm ROC matched < 3% Internal mode Q s > 2 x 10 6 Caltech data CSIRO data 26-April-06 LIGO - Georgia Tech 26
27 Core Optics installation and alignment 26-April-06 LIGO - Georgia Tech 27
28 Lock Acquisition 26-April-06 LIGO - Georgia Tech 28
29 Tidal Compensation Data Tidal evaluation 21-hour locked section of S1 data Predicted tides Feedforward Feedback Residual signal on voice coils Residual signal on laser 26-April-06 LIGO - Georgia Tech 29
30 Controlling angular degrees of freedom 26-April-06 LIGO - Georgia Tech 30
31 Interferometer Noise Limits Seismic Noise test mass (mirror) Quantum Noise Residual gas scattering "Shot" noise Radiation pressure LASER Wavelength & amplitude fluctuations Beam splitter photodiode 26-April-06 LIGO - Georgia Tech 31 Thermal (Brownian) Noise
32 What Limits LIGO Sensitivity? Seismic noise limits low frequencies Thermal Noise limits middle frequencies Quantum nature of light (Shot Noise) limits high frequencies Technical issues - alignment, electronics, acoustics, etc limit us before we reach these design goals 26-April-06 LIGO - Georgia Tech 32
33 Evolution of LIGO Sensitivity S1: 23 Aug 9 Sep 02 S2: 14 Feb 14 Apr 03 S3: 31 Oct 03 9 Jan 04 S4: 22 Feb 23 Mar 05 S5: 4 Nov April-06 LIGO - Georgia Tech 33
34 Commissioning /Running Time Line Inauguration First Lock Full Lock all IFO Now 4K strain noise x10-23 at 150 Hz [Hz -1/2 ] Engineering E2 Science E3 E5 E7 E8 E9 E10 E11 S1 S2 First Science Data S3 S4 S5 Runs 26-April-06 LIGO - Georgia Tech 34
35 Initial LIGO - Design Sensitivity 26-April-06 LIGO - Georgia Tech 35
36 Sensitivity Entering S5 Equivalent strain noise (Hz -1/2 ) Rms strain in 100 Hz BW: 0.4x10-21 H1, 20 Oct 05 L1, 30 Oct 05 SRD curve Frequency (Hz) 26-April-06 LIGO - Georgia Tech 36
37 S5 Run Plan and Outlook Interferometer duty cycles Goal is to collect at least a year s data of coincident operation at the science goal sensitivity Expect S5 to last about 1.5 yrs Run S2 S3 S4 S5 Target SRD goal L1 37% 22% 75% 85% 90% H1 74% 69% 81% 85% 90% H2 58% 63% 81% 85% 90% S5 is not completely hands-off 3- way 22% 16% 57% 70% 75% 26-April-06 LIGO - Georgia Tech 37
38 Sensitivity Entering S5 Hydraulic External Pre-Isolator 26-April-06 LIGO - Georgia Tech 38
39 Locking Problem is Solved 26-April-06 LIGO - Georgia Tech 39
40 What s after S5? 26-April-06 LIGO - Georgia Tech 40
41 Modest Improvements Now 14 Mpc Then 30 Mpc 26-April-06 LIGO - Georgia Tech 41
42 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 Signal stochastic background 26-April-06 LIGO - Georgia Tech 42
43 Compact Binary Collisions» Neutron Star Neutron Star waveforms are well described» Black Hole Black Hole need better waveforms» Search: matched templates chirps 26-April-06 LIGO - Georgia Tech 43
44 Template Bank Covers desired region of mass param space Calculated based on L1 noise curve Templates placed for max mismatch of δ = templates Second-order post-newtonian 26-April-06 LIGO - Georgia Tech 44
45 Optimal Filtering frequency domain Transform data to frequency domain : Generate template in frequency domain : ~ h ( f ) ~ s ( f ) Correlate, weighting by power spectral density of noise: ~ s ( f ) h S ( f ~ * h z( t) = 4 0 z( t) ( f ) ) Then inverse Fourier transform gives you the filter output at all times: ~ ~ s ( f ) h S ( f h ( f ) ) Find maxima of over arrival time and phase Characterize these by signal-to-noise ratio (SNR) and effective distance * e 2πi f t df 26-April-06 LIGO - Georgia Tech 45
46 Matched Filtering 26-April-06 LIGO - Georgia Tech 46
47 Inspiral Searches Mass BBH Search S3/S PBH MACHO S3/S4 BNS S3/S Spin is important Detection templates S3 High mass ratio Coming soon Physical waveform follow-up S3/S4 Inspiral-Burst S4 10 Mass
48 Binary Neutron Star Search Results (S2) Physical Review D, In Press cumulative number of events Rate < 47 per year per Milky-Way-like galaxy signal-to-noise ratio squared 26-April-06 LIGO - Georgia Tech 48
49 Binary Black Hole Search 26-April-06 LIGO - Georgia Tech 49
50 Binary Inspiral Search: LIGO Ranges inary neutron star range inary black hole range 26-April-06 LIGO - Georgia Tech Image: R. Powell 50
51 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 Signal stochastic background 26-April-06 LIGO - Georgia Tech 51
52 Unmodeled Bursts GOAL search for waveforms from sources for which we cannot currently make an accurate prediction of the waveform shape. METHODS Raw Data Time-domain high pass filter Time-Frequency Plane Search TFCLUSTERS Pure Time-Domain Search SLOPE frequency 8Hz 0.125s time 26-April-06 LIGO - Georgia Tech 52
53 Blind procedure gives one event candidate» Event immediately found to be correlated with airplane over-flight Burst Search Results 26-April-06 LIGO - Georgia Tech 53
54 Burst Source - Upper Limit 26-April-06 LIGO - Georgia Tech 54
55 Astrophysical Sources signatures 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 Signal stochastic background 26-April-06 LIGO - Georgia Tech 55
56 Detection of Periodic Sources Pulsars in our galaxy: periodic» search for observed neutron stars» all sky search (computing challenge)» r-modes Frequency modulation of signal due to Earth s motion relative to the Solar System Barycenter, intrinsic frequency changes. Amplitude modulation due to the detector s antenna pattern. 26-April-06 LIGO - Georgia Tech 56
57 Directed Pulsar Search 28 Radio Sources 26-April-06 LIGO - Georgia Tech 57
58 ALL SKY SEARCH enormous computing challenge LIGO Pulsar Search using home pc s BRUCE ALLEN Project Leader Univ of Wisconsin Milwaukee LIGO, UWM, AEI, APS 26-April-06 LIGO - Georgia Tech 58
59 All Sky Search Final S3 Data NO Events Observed 26-April-06 LIGO - Georgia Tech 59
60 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 Signal stochastic background 26-April-06 LIGO - Georgia Tech 60
61 Signals from the Early Universe Strength specified by ratio of energy density in GWs to total energy density needed to close the universe: Ω (f) GW = dρgw d(lnf) Detect by cross-correlating output of two GW detectors: ρ 1 critical Overlap Reduction Function 26-April-06 LIGO - Georgia Tech 61
62 Stochastic Background Search (S3) Fraction of Universe s energy in gravitational waves: (LIGO band) 26-April-06 LIGO - Georgia Tech 62
63 Results Stochastic Backgrounds 26-April-06 LIGO - Georgia Tech 63
64 LIGO works! Conclusions Data Analysis also works for broad range of science goals. Now making transition from limit setting to detection based analysis Data taking run (S5) to exploit Initial LIGO is well underway and will be complete within ~ 1.5 years Incremental improvements to follow S5 are being developed. (improve sensitivity ~ x2) Advanced LIGO fully approved by NSF and NSB and funding planned to commence in (design will improve sensitivity ~ x20) R&D on third generation detectors is underway 26-April-06 LIGO - Georgia Tech 64
65 Gravitational Wave Astronomy LIGO will provide a new way to view the dynamics of the Universe 26-April-06 LIGO - Georgia Tech 65
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