Astrophysical Sources of Gravitational Waves
... Directly detecting gravitational waves is the scientific goal for ground-based gravitational wave observatories located around the globe, including LIGO, the Laser Interferometer Gravitational-wave Observatory. LIGO has two 4 km-long interferometers: one is located in Hanford, Washington (Figure 2) ...
... Directly detecting gravitational waves is the scientific goal for ground-based gravitational wave observatories located around the globe, including LIGO, the Laser Interferometer Gravitational-wave Observatory. LIGO has two 4 km-long interferometers: one is located in Hanford, Washington (Figure 2) ...
Advanced LIGO: Context and Overview
... gravitational wave detectors have started observations, and are already yielding data that are being interpreted to establish new upper limits on gravitational-wave flux. The sensitivity of the initial LIGO instruments is such that it is perfectly possible that discoveries will be made. If they succ ...
... gravitational wave detectors have started observations, and are already yielding data that are being interpreted to establish new upper limits on gravitational-wave flux. The sensitivity of the initial LIGO instruments is such that it is perfectly possible that discoveries will be made. If they succ ...
G030164-00 - DCC
... Despite their immense technical challenges, the initial LIGO IFO’s were designed conservatively, based on “tabletop” prototypes, but with expected sensitivity gain of ~1000. Given the expected low rate of detectable GW events, it was always planned that in engineering, building and commissioning ini ...
... Despite their immense technical challenges, the initial LIGO IFO’s were designed conservatively, based on “tabletop” prototypes, but with expected sensitivity gain of ~1000. Given the expected low rate of detectable GW events, it was always planned that in engineering, building and commissioning ini ...
PPT - LSC
... • The direction as well as the time of the event are known beforehand • All band electromagnetic detectors from radio to ultrahigh energy gamma rays • Possible neutrino detectors • Tune the high frequency gravitational wave detectors to catch ISCO, QNM and so on ...
... • The direction as well as the time of the event are known beforehand • All band electromagnetic detectors from radio to ultrahigh energy gamma rays • Possible neutrino detectors • Tune the high frequency gravitational wave detectors to catch ISCO, QNM and so on ...
LIGO: The Portal to Spacetime - Hanford Observatory
... The Nature of Gravitational Collapse and Its Outcomes "Since I first embarked on my study of general relativity, gravitational collapse has been for me the most compelling implication of the theory - indeed the most compelling idea in all of physics . . . It teaches us that space can be crumpled li ...
... The Nature of Gravitational Collapse and Its Outcomes "Since I first embarked on my study of general relativity, gravitational collapse has been for me the most compelling implication of the theory - indeed the most compelling idea in all of physics . . . It teaches us that space can be crumpled li ...
UWB2002 - LIGO Hanford Observatory
... Gravitational Radiation Confirmed In 1974, J. Taylor and R. Hulse discovered a pulsar orbiting a companion neutron star. This “binary pulsar” provides some of the best tests of General Relativity. Theory predicts the orbital period of 8 hours should change as energy is carried away by gravitational ...
... Gravitational Radiation Confirmed In 1974, J. Taylor and R. Hulse discovered a pulsar orbiting a companion neutron star. This “binary pulsar” provides some of the best tests of General Relativity. Theory predicts the orbital period of 8 hours should change as energy is carried away by gravitational ...
initial LIGO construction,
... sensitivity to gravitational wave sources in a new frequency regime by two to three decades in amplitude and bandwidth from all previous searches Although the existence of gravitational radiation is not a unique property of General Relativity, that theory makes a number of unambiguous predictions ab ...
... sensitivity to gravitational wave sources in a new frequency regime by two to three decades in amplitude and bandwidth from all previous searches Although the existence of gravitational radiation is not a unique property of General Relativity, that theory makes a number of unambiguous predictions ab ...
Australia-France PhD projects
... o Key questions: what is the beaming angle of GRBs? What is the nature of the progenitors? How are GRBs connected to supernovae? Population studies of GRBs. o Key questions: what is the rate GRBs in the universe? What fraction of GRBs can be detected by gravitational wave detectors? Are afterglows ...
... o Key questions: what is the beaming angle of GRBs? What is the nature of the progenitors? How are GRBs connected to supernovae? Population studies of GRBs. o Key questions: what is the rate GRBs in the universe? What fraction of GRBs can be detected by gravitational wave detectors? Are afterglows ...
Recovering Injections Poster
... 1. Carnegie Mellon University, Pittsburgh, PA. 2. California Institute of Technology, Pasadena, CA. 3. Jet Propulsion Laboratory, Pasadena, CA. ...
... 1. Carnegie Mellon University, Pittsburgh, PA. 2. California Institute of Technology, Pasadena, CA. 3. Jet Propulsion Laboratory, Pasadena, CA. ...
G030139-00 - DCC
... Advanced LIGO: ~2.5 hours = 1 year of Initial LIGO » Volume of sources grows with cube of sensitivity » >10x in sensitivity; ~ 3000 in rate ...
... Advanced LIGO: ~2.5 hours = 1 year of Initial LIGO » Volume of sources grows with cube of sensitivity » >10x in sensitivity; ~ 3000 in rate ...
G070666-00 - DCC
... Factor of ~10 better than current LIGO factor of ~1000 in volume ! 2007/10/26 – LAPP Annecy ...
... Factor of ~10 better than current LIGO factor of ~1000 in volume ! 2007/10/26 – LAPP Annecy ...
IndIGO Indian Initiative in Gravitational
... IndIGO 3m Prototype Detector Funded by TIFR Mumbai on campus (2010)PI: C. S.Unnikrishnan ( INR 3.5cr ~.7 M$ ) Goals of the TIFR 3-m prototype interferometer (to be operational in 2014): ...
... IndIGO 3m Prototype Detector Funded by TIFR Mumbai on campus (2010)PI: C. S.Unnikrishnan ( INR 3.5cr ~.7 M$ ) Goals of the TIFR 3-m prototype interferometer (to be operational in 2014): ...
DCC - LIGO Document Control Center Portal
... LIGO finished S5 Science run enhanced LIGO upgrade is happening advanced LIGO is beginning modulation challenges are understood/solved Gravitational wave detection pushes state-of-the art in CW solid state laser technology, optical fabrication and metrology, and control systems ...
... LIGO finished S5 Science run enhanced LIGO upgrade is happening advanced LIGO is beginning modulation challenges are understood/solved Gravitational wave detection pushes state-of-the art in CW solid state laser technology, optical fabrication and metrology, and control systems ...
T1100458
... in the "USER" section, the status should read "DRIVER DISABLED" On the controller front panel: the "IDLE" LED should be lit the "Enable" LED should be off the “ON” LED should be on ...
... in the "USER" section, the status should read "DRIVER DISABLED" On the controller front panel: the "IDLE" LED should be lit the "Enable" LED should be off the “ON” LED should be on ...
E0900349-v12_ETM-Tel-Secondary_Parabolic Specification
... Edge orientation mark shall be placed to indicate maximum edge thickness within rotational tolerance of 1 deg, as shown in figure 1: 0.24 +/- 0.1 mm wide x FULL BARREL LENGTH. ADDITIONAL MARKING @ 90 Deg. intervals +/-2 Degrees, on barrel, and on back face (full diameter length) as shown in Figure:2 ...
... Edge orientation mark shall be placed to indicate maximum edge thickness within rotational tolerance of 1 deg, as shown in figure 1: 0.24 +/- 0.1 mm wide x FULL BARREL LENGTH. ADDITIONAL MARKING @ 90 Deg. intervals +/-2 Degrees, on barrel, and on back face (full diameter length) as shown in Figure:2 ...
G060226-00_part2 - DCC
... Motivation: » Arm length fluctuations are dominated by low frequency motions, f < 0.5 Hz; motion in this band (~100 nm-rms) not expected to be much lower than in initial LIGO (@LLO, w/ HEPI) » Reducing this rms by another factor of 10-100x could: – Make lock acquisition much simpler – Enable lock ...
... Motivation: » Arm length fluctuations are dominated by low frequency motions, f < 0.5 Hz; motion in this band (~100 nm-rms) not expected to be much lower than in initial LIGO (@LLO, w/ HEPI) » Reducing this rms by another factor of 10-100x could: – Make lock acquisition much simpler – Enable lock ...
Particle Astrophysics Advisory Panel Balance of Programme Exercise
... Particle astrophysics (PA) has seen enormous advances over the last few years. These include the first observation of gravitational waves from binary black hole mergers, by Advanced LIGO, with its subsequent opening of a new field of astrophysics. Construction has begun on second generation dark mat ...
... Particle astrophysics (PA) has seen enormous advances over the last few years. These include the first observation of gravitational waves from binary black hole mergers, by Advanced LIGO, with its subsequent opening of a new field of astrophysics. Construction has begun on second generation dark mat ...
Overview of LIGO core technologies - Gravitational Waves
... produces a tiny strain h = ∆L / L § We measure ∆φ = 4π ∆L/λlaser = 4π L h /λ laser so to measure small h, need large L § But not too large! If L > λ g/4, GW changes sign while laser light is still in arms, cancelling effect on ∆φ § Optimal: L > λ g/4 ~ 750 km. But not very practical! § For more prac ...
... produces a tiny strain h = ∆L / L § We measure ∆φ = 4π ∆L/λlaser = 4π L h /λ laser so to measure small h, need large L § But not too large! If L > λ g/4, GW changes sign while laser light is still in arms, cancelling effect on ∆φ § Optimal: L > λ g/4 ~ 750 km. But not very practical! § For more prac ...
G080363-00 - DCC
... Smaller diffraction-limited Gaussian beams Much wider mesa beams possible • Additional TN Gain of 4-5 • 10-20 x more light required • More radiation pressure noise ...
... Smaller diffraction-limited Gaussian beams Much wider mesa beams possible • Additional TN Gain of 4-5 • 10-20 x more light required • More radiation pressure noise ...
G030009-00 - DCC
... about space, time and the nuclear equation of state What was the universe like in the earliest moments of the big bang? What surprises have we yet to discover about our universe? LIGO-G030009-00-W ...
... about space, time and the nuclear equation of state What was the universe like in the earliest moments of the big bang? What surprises have we yet to discover about our universe? LIGO-G030009-00-W ...
G000175-00 - DCC
... International network (LIGO, Virgo, GEO, TAMA and AIGO) enable locating sources and decomposing polarization of ...
... International network (LIGO, Virgo, GEO, TAMA and AIGO) enable locating sources and decomposing polarization of ...
Advanced LIGO—the Next Generation
... Newtonian background is limit for ground-based detectors (~10 Hz) » Time-varying distribution of mass in vicinity of test mass » Seismic compression, rarefaction of earth dominates » Advanced LIGO targeted to reach this limit for our sites ...
... Newtonian background is limit for ground-based detectors (~10 Hz) » Time-varying distribution of mass in vicinity of test mass » Seismic compression, rarefaction of earth dominates » Advanced LIGO targeted to reach this limit for our sites ...
LIGO
LIGO, which stands for the Laser Interferometer Gravitational-Wave Observatory, is a large-scale physics experiment aiming to directly detect gravitational waves. Cofounded in 1992 by Kip Thorne and Ronald Drever of Caltech and Rainer Weiss of MIT, LIGO is a joint project between scientists at MIT, Caltech, and many other colleges and universities. It is sponsored by the National Science Foundation (NSF). At the cost of $620 million, it is the largest and most ambitious project ever funded by the NSF.Observations at LIGO began in 2002, ended in 2010, and no gravitational waves have been reported. The original detectors were disassembled and were replaced by improved versions known as ""Advanced LIGO"". As of February 2015, two such advanced detectors (one in Livingston, Louisiana and the other in Hanford, Washington) have been brought into engineering mode. On September 18, 2015, Advanced LIGO became fully operational and began formal science operations at twice the sensitivity of the initial LIGO interferometers.