LIGO-G000306-00-M LIGO and Detection of Gravitational Waves Barry Barish 13 October 2000.

Slides:



Advertisements
Similar presentations
Dennis Ugolini, Trinity University Bite of Science Session, TEP 2014 February 13, 2014 Catching the Gravitational Waves.
Advertisements

Laser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011 LIGO-G v1.
The 2000 Buhl Lecture Einstein’s Unfinished Symphony: “Listening” for Gravitational Waves Barry C. Barish.
LIGO-G M First Generation Interferometers Barry Barish 30 Oct 2000 Workshop on Astrophysical Sources for Ground-Based Gravitational Wave Detectors.
Gravitational Waves Laser Interferometric Detectors
1 Science Opportunities for Australia Advanced LIGO Barry Barish Director, LIGO Canberra, Australia 16-Sept-03 LIGO-G M.
LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
LIGO Status and Plans Barry Barish / Gary Sanders 13-May-02
LIGO-G9900XX-00-M LIGO Status and Plans Barry Barish 5 June 2000 Gravitational Waves: A Challenge to Theoretical Astrophysics Trieste, 5-9 June 2000.
Status of the LIGO Project
2/9/2006Welcome to LIGO1 Welcome to LIGO!. 2/9/2006Welcome to LIGO2 LIGO: A detector that measures very tiny displacements How tiny?
The LIGO Project ( Laser Interferometer Gravitational-Wave Observatory) Rick Savage - LIGO Hanford Observatory.
Barry Barish AIP Conference, Sydney Australia 11-July-02
Probing the Universe for Gravitational Waves Barry C. Barish Caltech Cornell University 3-April-06 Crab Pulsar.
1 Einstein's Legacy: General Relativity, our Best Description of the Universe Barry C. Barish Caltech LLNL Science Day 23-May-05.
Einstein’s Theory of Gravitation “instantaneous action at a distance”
Newton Universal Gravitation
LIGO Present and Future
Detecting Gravitational Waves: How does LIGO work and how well does LIGO work? Barry C. Barish Caltech University of Kentucky 4-March-05 "Colliding.
The Search for Gravitational Waves Barry Barish Caltech University of Iowa 16-Sept-02.
G M LIGO “First Lock” Barry Barish 21 October 2000.
LIGO-G W Commissioning Data on Vibration Isolation & Suspensions Fred Raab 24 October 02.
LIGO-G W "Colliding Black Holes" Credit: National Center for Supercomputing Applications (NCSA) Searching for Gravitational Waves with LIGO Reported.
Laser Interferometer Gravitational-wave Observatory LIGO
LIGO-G9900XX-00-M LIGO: Progress and Prospects Barry Barish 18 July 2000 COSPAR 2000 Fundamental Physics in Space.
1 Observing the Most Violent Events in the Universe Virgo Barry Barish Director, LIGO Virgo Inauguration 23-July-03 Cascina 2003.
Listening to Gravitational Waves: Einstein’s Songlines from the Universe Barry C. Barish.
LIGO-G M LIGO and Prospects for Detection of Gravitational Waves Barry Barish 1 November 2000.
Sir Isaac Newton Universal Gravitation
LIGO-G9900XX-00-M LIGO Status and Plans Barry Barish March 13, 2000.
Catching the Waves with LIGO Barry Barish Los Alamos National Laboratory 27-March-03.
Overview Ground-based Interferometers Barry Barish Caltech Amaldi-6 20-June-05.
The LIGO Project ( Laser Interferometer Gravitational-Wave Observatory) Rick Savage - LIGO Hanford Observatory.
Probing the Universe for Gravitational Waves Barry C. Barish Caltech Georgia Tech 26-April-06 Crab Pulsar.
LIGO-G9900XX-00-M LIGO and Detection of Gravitational Waves Barry Barish 14 September 2000.
LIGO -- Studying the Fabric of the Universe LIGO-GOxxxx Barry C. Barish National Science Board LIGO Livingston, LA 4-Feb-04.
David Shoemaker 30 August 05
LIGO-G W Status of LIGO Installation and Commissioning Frederick J. Raab, LIGO Hanford Observatory.
LIGO-G v1 The LIGO Vacuum System and plans for LIGO-Australia Stan Whitcomb IndIGO - ACIGA meeting on LIGO-Australia 9 February 2011.
1 G Mike Smith Gravitational Waves & Precision Measurements.
The GEO 600 Detector Andreas Freise for the GEO 600 Team Max-Planck-Institute for Gravitational Physics University of Hannover May 20, 2002.
Gravitational Wave Arezu Dehghafnar Physics Department SUT.
LIGO-G Black holes, Einstein, and space-time ripples Peter R. Saulson Syracuse University.
14 July LNGSSearch for Gravitational Waves with Interferometers 1 The search for gravitational waves with the new generation of interferometers Peter.
LIGO-G D Enhanced LIGO Kate Dooley University of Florida On behalf of the LIGO Scientific Collaboration SESAPS Nov. 1, 2008.
LIGO- G D Status of LIGO Stan Whitcomb ACIGA Workshop 21 April 2004.
Koji Arai – LIGO Laboratory / Caltech LIGO-G v1.
LIGO-G D The LIGO-I Gravitational-wave Detectors Stan Whitcomb CaJAGWR Seminar February 16, 2001.
LIGO- G D The LIGO Instruments Stan Whitcomb NSB Meeting LIGO Livingston Observatory 4 February 2004.
Advanced interferometers for astronomical observations Lee Samuel Finn Center for Gravitational Wave Physics, Penn State.
LIGO-G W "Colliding Black Holes" Credit: National Center for Supercomputing Applications (NCSA) The Laser Interferometer Gravitational-Wave Observatory.
Initial and Advanced LIGO Detectors
Gravitational Waves.
LIGO-G D Searching for Gravitational Waves with LIGO (Laser Interferometer Gravitational-wave Observatory) Stan Whitcomb LIGO/Caltech National.
LIGO-G D LIGO Laboratory1 Stoyan Nikolov LIGO-G D The LIGO project’s quest for gravitational waves Presenting LIGO to the students of.
LIGO-G M The Curtain Rises on LIGO: Listening to Einstein's Gravitational Symphony Gary Sanders Laser Interferometer Gravitational Wave Observatory.
LIGO-G M Scientific Operation of LIGO Gary H Sanders LIGO Laboratory California Institute of Technology APS Meeting APR03, Philadelphia Gravitational-Wave.
LIGO-G M Catching the Waves with LIGO Barry Barish 26 Sept 01.
LIGO G M Intro to LIGO Seismic Isolation Pre-bid meeting Gary Sanders LIGO/Caltech Stanford, April 29, 2003.
LIGO-G M Press Conference Scientific Operation of LIGO Gary H Sanders Caltech (on behalf of a large team) APS April Meeting Philadelphia 6-April-03.
The quest for Gravitation Waves By Benjamin Thayer.
Searches for Gravitational Waves Barry Barish Caltech IPA London – Aug 2014 “Merging Neutron Stars“ (Price & Rosswog)
The search for those elusive gravitational waves
The Laser Interferometer Gravitational-Wave Observatory In Operation
The Search for Gravitational Waves with Advanced LIGO
Is there a future for LIGO underground?
Nergis Mavalvala MIT IAU214, August 2002
Gravity -- Studying the Fabric of the Universe Barry C
Status of LIGO Installation and Commissioning
Squeezed Light Techniques for Gravitational Wave Detection
Presentation transcript:

LIGO-G M LIGO and Detection of Gravitational Waves Barry Barish 13 October 2000

LIGO-G M Einstein’s Theory of Gravitation Newton’s Theory “instantaneous action at a distance” Einstein’s Theory information carried by gravitational radiation at the speed of light

LIGO-G M Imagine space as a stretched rubber sheet. A mass on the surface will cause a deformation. Another mass dropped onto the sheet will roll toward that mass. Einstein theorized that smaller masses travel toward larger masses, not because they are "attracted" by a mysterious force, but because the smaller objects travel through space that is warped by the larger object. Einstein’s warpage of spacetime

LIGO-G M Predict the bending of light passing in the vicinity of the massive objects First observed during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster Their measurements showed that the light from these stars was bent as it grazed the Sun, by the exact amount of Einstein's predictions. The light never changes course, but merely follows the curvature of space. Astronomers now refer to this displacement of light as gravitational lensing.

LIGO-G M Einstein’s Theory of Gravitation experimental tests “Einstein Cross” The bending of light rays gravitational lensing Quasar image appears around the central glow formed by nearby galaxy. The Einstein Cross is only visible in southern hemisphere. In modern astronomy, such gravitational lensing images are used to detect a ‘dark matter’ body as the central object

LIGO-G M Einstein’s Theory of Gravitation experimental tests Mercury’s orbit perihelion shifts forward twice Newton’s theory Mercury's elliptical path around the Sun shifts slightly with each orbit such that its closest point to the Sun (or "perihelion") shifts forward with each pass. Astronomers had been aware for two centuries of a small flaw in the orbit, as predicted by Newton's laws. Einstein's predictions exactly matched the observation.

LIGO-G M Einstein’s Theory of Gravitation gravitational waves a necessary consequence of Special Relativity with its finite speed for information transfer Einstein in 1916 and 1918 put forward the formulation of gravitational waves in General Relativity time dependent gravitational fields 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

LIGO-G M 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 . 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 The strain h  takes the form of a plane wave propagating with 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.

LIGO-G M Gravitational Waves the evidence Neutron Binary System PSR Timing of pulsars   17 / sec ~ 8 hr

LIGO-G M Hulse and Taylor results & due to loss of orbital energy & period speeds up 25 sec from & measured to ~50 msec accuracy & deviation grows quadratically with time emission of gravitational waves

LIGO-G M Radiation of Gravitational Waves Radiation of gravitational waves from binary inspiral system LISA the center of the triangle formation will be in the ecliptic plane 1 AU from the Sun and 20 degrees behind the Earth.

LIGO-G M Astrophysics Sources frequency range  EM waves are studied over ~20 orders of magnitude »(ULF radio  HE  rays)  Gravitational Waves over ~10 orders of magnitude » (terrestrial + space) Audio band

LIGO-G M Suspended mass Michelson-type interferometers on earth’s surface detect distant astrophysical sources International network (LIGO, Virgo, GEO, TAMA) enable locating sources and decomposing polarization of gravitational waves. Interferometers terrestrial

LIGO-G M Detection of Gravitational Waves interferometry suspended test masses Michelson Interferometer Fabry-Perot Arm Cavities LIGO (4 km), stretch (squash) = m will be detected at frequencies of 10 Hz to 10 4 Hz. It can detect waves from a distance of light years

LIGO-G M Detection of Gravitational Waves Interferometry – folded arms Folded arms – long light paths Schemes - delay line is simple but requires large mirrors - power recycling mirrors small, but harder controls problems  msec

LIGO-G M Detection of Gravitational Waves Interferometry – folded arms Power recycled Michelson Interferometer with Fabry-Perot arms arm cavities store light for ~ 100 round trips or ~ 3 msec power recycling re-uses light heading back to the laser giving an additional factor of x30

LIGO-G M LIGO Interferometers Laser end test mass 4 km (2 km) Fabry-Perot arm cavity recycling mirror input test mass beam splitter Power Recycled Michelson Interferometer with Fabry-Perot Arm Cavities Power Recycled Michelson Interferometer with Fabry-Perot Arm Cavities signal

LIGO-G M LIGO I the noise floor  Interferometry is limited by three fundamental noise sources  seismic noise at the lowest frequencies  thermal noise at intermediate frequencies  shot noise at high frequencies  Many other noise sources lurk underneath and must be controlled as the instrument is improved

LIGO-G M Noise Floor 40 m prototype displacement sensitivity in 40 m prototype. comparison to predicted contributions from various noise sources sensitivity demonstration

LIGO-G M Phase Noise splitting the fringe spectral sensitivity of MIT phase noise interferometer above 500 Hz shot noise limited near LIGO I goal additional features are from 60 Hz powerline harmonics, wire resonances (600 Hz), mount resonances, etc expected signal  radians phase shift demonstration experiment

LIGO-G M LIGO I interferometer LIGO I configuration Science Run

LIGO-G M LIGO I the noise floor  Interferometry is limited by three fundamental noise sources  seismic noise at the lowest frequencies  thermal noise at intermediate frequencies  shot noise at high frequencies  Many other noise sources lurk underneath and must be controlled as the instrument is improved

LIGO-G M LIGO astrophysical sources LIGO I ( ) LIGO II (2007- ) Advanced LIGO

LIGO-G M Interferometers international network LIGO Simultaneously detect signal (within msec) detection confidence locate the sources decompose the polarization of gravitational waves GEO Virgo TAMA AIGO

LIGO-G M LIGO Sites Livingston Observatory Hanford Observatory

LIGO-G M LIGO Livingston Observatory

LIGO-G M LIGO Hanford Observatory

LIGO-G M LIGO Plans schedule 1996Construction Underway (mostly civil) 1997Facility Construction (vacuum system) 1998Interferometer Construction (complete facilities) 1999Construction Complete (interferometers in vacuum) 2000Detector Installation (commissioning subsystems) 2001 Commission Interferometers (first coincidences) 2002Sensitivity studies (initiate LIGOI Science Run) LIGO I data run (one year integrated data at h ~ ) 2005Begin LIGO II installation

LIGO-G M LIGO Facilities Beam Tube Enclosure minimal enclosure reinforced concrete no services

LIGO-G M LIGO Beam Tube  LIGO beam tube under construction in January 1998  65 ft spiral welded sections  girth welded in portable clean room in the field 1.2 m diameter - 3mm stainless 50 km of weld NO LEAKS !!

LIGO-G M Beam Tube bakeout I = 2000 amps for ~ 1 week no leaks !! final vacuum at level where not limiting noise, even for future detectors

LIGO-G M LIGO I the noise floor  Interferometry is limited by three fundamental noise sources  seismic noise at the lowest frequencies  thermal noise at intermediate frequencies  shot noise at high frequencies  Many other noise sources lurk underneath and must be controlled as the instrument is improved

LIGO-G M LIGO vacuum equipment

LIGO-G M Vacuum Chambers Vibration Isolation Systems »Reduce in-band seismic motion by orders of magnitude »Compensate for microseism at 0.15 Hz by a factor of ten »Compensate (partially) for Earth tides

LIGO-G M Seismic Isolation Springs and Masses damped spring cross section

LIGO-G M Seismic Isolation performance Horizontal Vertical HAM stack in air BSC stack in vacuum

LIGO-G M Seismic Isolation suspension system support structure is welded tubular stainless steel suspension wire is 0.31 mm diameter steel music wire fundamental violin mode frequency of 340 Hz suspension assembly for a core optic

LIGO-G M LIGO Noise Curves modeled wire resonances

LIGO-G M Core Optics fused silica Caltech data CSIRO data  Surface uniformity < 1 nm rms  Scatter < 50 ppm  Absorption < 2 ppm  ROC matched < 3%  Internal mode Q’s > 2 x 10 6

LIGO-G M Core Optics Suspension

LIGO-G M Core Optics Installation and Alignment

LIGO-G M LIGO Laser  Nd:YAG   m  Output power > 8W in TEM00 mode

LIGO-G M Laser stabilization IO 10-Watt Laser PSL Interferometer 15m 4 km TidalWideband  Deliver pre-stabilized laser light to the 15-m mode cleaner Frequency fluctuations In-band power fluctuations Power fluctuations at 25 MHz  Provide actuator inputs for further stabilization Wideband Tidal Hz/Hz 1/ Hz/ Hz 1/ Hz/ Hz 1/2

LIGO-G M Prestabalized Laser performance  > 18,000 hours continuous operation  Frequency and lock very robust  TEM 00 power > 8 watts  Non-TEM 00 power < 10%

LIGO-G M Commissioning Configurations  Mode cleaner and Pre-Stabilized Laser  2km one-arm cavity  short Michelson interferometer studies  Lock entire Michelson Fabry-Perot interferometer “FIRST LOCK”

LIGO-G M Detector Commissioning: 2-km Arm Test  12/99 – 3/00  Alignment “dead reckoning” worked  Digital controls, networks, and software all worked  Exercised fast analog laser frequency control  Verified that core optics meet specs  Long-term drifts consistent with earth tides

LIGO-G M Confirmation of Initial Alignment  Opening gate valves revealed alignment “dead reckoned” from corner station was within 100 micro radians beam spot

LIGO-G M Locking the Long Arm  12/1/99 Flashes of light  12/9/ seconds lock  1/14/00 2 seconds lock  1/19/00 60 seconds lock  1/21/00 5 minutes lock (on other arm)  2/12/00 18 minutes lock  3/4/00 90 minutes lock (temperature stabilized laser reference cavity)  3/26/00 10 hours lock First interference fringes from the 2-km arm

LIGO-G M locked long arm alignment - wavefront sensors Alignment fluctuations before engaging wavefront sensors After engaging wavefront sensors

LIGO-G M 2km Fabry-Perot cavity 15 minute locked stretch

LIGO-G M Locked long arm long term effects 10 hour locked section Stretching consistent with earth tides

LIGO-G M Near-Michelson interferometer Interference fringes from the power recycled near Michelson interferometer power recycled (short) Michelson Interferometer employs full mixed digital/analog servos

LIGO-G M Complete Interferometer locking Interferometer lock states

LIGO-G M Brief Locked Stretch X arm Reflected light Y arm Anti-symmetric port

LIGO-G M Significant Events

LIGO-G M Chirp Signal binary inspiral distance from the earth r masses of the two bodies orbital eccentricity e and orbital inclination i determine

LIGO-G M LIGO astrophysical sources Compact binary mergers LIGO sensitivity to coalescing binaries

LIGO-G M LIGO Sites Hanford Observatory Livingston Observatory

LIGO-G M Detection Strategy Coincidences  Two Sites - Three Interferometers »Single Interferometernon-gaussian level~50/hr »Hanford (Doubles) correlated rate (x1000)~1/day »Hanford + Livingston uncorrelated (x5000)<0.1/yr  Data Recording (time series) »gravitational wave signal (0.2 MB/sec) »total data (16 MB/s) »on-line filters, diagnostics, data compression »off line data analysis, archive etc  Signal Extraction »signal from noise (vetoes, noise analysis) »templates, wavelets, etc

LIGO-G M Interferometer Data 40 m Real interferometer data is UGLY!!! (Gliches - known and unknown) LOCKING RINGING NORMAL ROCKING

LIGO-G M The Problem How much does real data degrade complicate the data analysis and degrade the sensitivity ?? Test with real data by setting an upper limit on galactic neutron star inspiral rate using 40 m data

LIGO-G M “Clean up” data stream Effect of removing sinusoidal artifacts using multi-taper methods Non stationary noise Non gaussian tails

LIGO-G M Inspiral ‘Chirp’ Signal Template Waveforms “matched filtering” 687 filters 44.8 hrs of data 39.9 hrs arms locked 25.0 hrs good data sensitivity to our galaxy h ~ mHz -1/2 expected rate ~10 -6 /yr

LIGO-G M Detection Efficiency Simulated inspiral events provide end to end test of analysis and simulation code for reconstruction efficiency Errors in distance measurements from presence of noise are consistent with SNR fluctuations

LIGO-G M Setting a limit Upper limit on event rate can be determined from SNR of ‘loudest’ event Limit on rate: R < 0.5/hour with 90% CL  = 0.33 = detection efficiency An ideal detector would set a limit: R < 0.16/hour

LIGO-G M gravitational waves ’s light Supernova

LIGO-G M Supernovae Gravitational Waves Non axisymmetric collapse ‘burst’ signal Rate 1/50 yr - our galaxy 3/yr - Virgo cluster

LIGO-G M kick sequencegravitational core collapse Model of Core Collapse A. Burrows et al

LIGO-G M pulsar proper motions Velocities -  young SNR(pulsars?)  > 500 km/sec Burrows et al  recoil velocity of matter and neutrinos Asymmetric Collapse?

LIGO-G M LIGO astrophysical sources

LIGO-G M LIGO astrophysical sources  Pulsars in our galaxy »non axisymmetric: 10-4 <  < 10-6 »science: neutron star precession; interiors »narrow band searches best

LIGO-G M Sources of Gravitational Waves ‘Murmurs’ from the Big Bang signals from the early universe Cosmic microwave background

LIGO-G M Conclusions  LIGO I construction complete  LIGO I commissioning and testing ‘on track’  “First Lock” will be officially established 20 Oct 00  Data analysis schemes are being developed, including tests with 40 m data  First Science Run will begin during 2002  Significant improvements in sensitivity anticipated to begin about 2006