Slide 1
... With these techniques, we have demonstrated squeezing-enhancement (an increase in S/N) in the LIGO prototype interferometer by about 3dB in the shot-noise-limited frequency band (above 40kHz) This squeezer is applicable to any interferometer configuration with DC readout. ...
... With these techniques, we have demonstrated squeezing-enhancement (an increase in S/N) in the LIGO prototype interferometer by about 3dB in the shot-noise-limited frequency band (above 40kHz) This squeezer is applicable to any interferometer configuration with DC readout. ...
Physics of LIGO, lecture 1a
... University of Western Australia University of Wisconsin-Milwaukee Washington State University ...
... University of Western Australia University of Wisconsin-Milwaukee Washington State University ...
DC Readout Experiment at the Caltech 40m
... transmissivity mismatch been determined to be 10% by a fit to the data. We also present the results of measurements of oscillator phase and amplitude noise couplings, but we do not currently have modeling tools for these. 3.2.1. Laser Frequency Noise The 40m interferometer is equipped with a Common ...
... transmissivity mismatch been determined to be 10% by a fit to the data. We also present the results of measurements of oscillator phase and amplitude noise couplings, but we do not currently have modeling tools for these. 3.2.1. Laser Frequency Noise The 40m interferometer is equipped with a Common ...
1. Introduction
... Virgo on each others analysis methods as performed within their respective collaborations. This work has now been expanded to include a joint search for stochastic gravitational waves. Stochastic gravitational waves can be thought of as a gravitational wave equivalent of the cosmic microwave backgro ...
... Virgo on each others analysis methods as performed within their respective collaborations. This work has now been expanded to include a joint search for stochastic gravitational waves. Stochastic gravitational waves can be thought of as a gravitational wave equivalent of the cosmic microwave backgro ...
G040134-00 - DCC
... Clearances & mass margins are tight! » Requires close coordination between groups & iteration in layout & subsystem design; can’t a’ priori define a set of immutable requirements » Requires coupled structural dynamics analysis of all payloads attached to the SEI » Requires Systems maintenance of mas ...
... Clearances & mass margins are tight! » Requires close coordination between groups & iteration in layout & subsystem design; can’t a’ priori define a set of immutable requirements » Requires coupled structural dynamics analysis of all payloads attached to the SEI » Requires Systems maintenance of mas ...
Port - LIGO
... Advanced LIGO • Design needs to take into account alignment sensing as well as length sensing • Current design of control system is optimized only with respect to sideband power in the recycling cavities • We find that high power levels do not guarantee optimal alignment signals • We propose changes ...
... Advanced LIGO • Design needs to take into account alignment sensing as well as length sensing • Current design of control system is optimized only with respect to sideband power in the recycling cavities • We find that high power levels do not guarantee optimal alignment signals • We propose changes ...
IndIGO Indian Initiative in Gravitational-wave Observations
... Large Data Analysis Center Facilities are being planned under the next five year plan for consolidated IndIGO participation in LSC for Advanced LIGO ...
... Large Data Analysis Center Facilities are being planned under the next five year plan for consolidated IndIGO participation in LSC for Advanced LIGO ...
M.Evans - LIGO
... » back of the envelope is not large enough » complex hardware : pre-stabilized laser, input optics, core optics, seismic isolation system on moving ground, suspension, sensors and actuators » feedback loops : length and alignment controls, feedback to laser » non-linearity : cavity dynamics to actua ...
... » back of the envelope is not large enough » complex hardware : pre-stabilized laser, input optics, core optics, seismic isolation system on moving ground, suspension, sensors and actuators » feedback loops : length and alignment controls, feedback to laser » non-linearity : cavity dynamics to actua ...
Enhanced sensitivity of the LIGO gravitational The LIGO Scientific Collaboration*
... the most promising astrophysical sources, such as coalescences of black hole and neutron star binary systems, but also poses a significant experimental challenge. Seismic motion is huge compared to the desired sensitivity, albeit at very low frequencies of less than 1 Hz, and LIGO employs a very hig ...
... the most promising astrophysical sources, such as coalescences of black hole and neutron star binary systems, but also poses a significant experimental challenge. Seismic motion is huge compared to the desired sensitivity, albeit at very low frequencies of less than 1 Hz, and LIGO employs a very hig ...
Input Optic requirements and components for High Power lasers
... » DC-sensing (now baseline): RF signals are used only for auxiliary d.o.f.s – Requirements unclear. Complicated function of locking scheme, cross coupling between channels, noise spectrum, and feedback bandwidth. But will be less difficult than in RF sensing. ...
... » DC-sensing (now baseline): RF signals are used only for auxiliary d.o.f.s – Requirements unclear. Complicated function of locking scheme, cross coupling between channels, noise spectrum, and feedback bandwidth. But will be less difficult than in RF sensing. ...
IndIGO Indian Initiative in Gravitational
... membership in LIGO Scientific Collaboration (LSC) for participation in Advanced LIGO. • Create a Tier-2 data centre in IUCAA for LIGO Scientific Collaboration Deliverables and as a LSC Resource • July 2011 IndIGO Consortium Application for Gravitational Wave International Committee (GWIC) Accepted. ...
... membership in LIGO Scientific Collaboration (LSC) for participation in Advanced LIGO. • Create a Tier-2 data centre in IUCAA for LIGO Scientific Collaboration Deliverables and as a LSC Resource • July 2011 IndIGO Consortium Application for Gravitational Wave International Committee (GWIC) Accepted. ...
Havana, 12 January, 2017 Dear Colleague This
... GRAVITATIONAL WAVE OBSERVATORIES AND DETECTORS: GEO600 - GEO600 Gravitational Wave Detector; LIGO - The Laser Interferometer Gravitational-Wave Observatory; LISA - Gravitational-Wave Observatory; NA61/SHINE/CERN Detector; VIRGO - Virgo Detector for Gravitational Waves. LABORATORIES: FERMILAB – Fermi ...
... GRAVITATIONAL WAVE OBSERVATORIES AND DETECTORS: GEO600 - GEO600 Gravitational Wave Detector; LIGO - The Laser Interferometer Gravitational-Wave Observatory; LISA - Gravitational-Wave Observatory; NA61/SHINE/CERN Detector; VIRGO - Virgo Detector for Gravitational Waves. LABORATORIES: FERMILAB – Fermi ...
ExpandHorizons_06 - Hanford
... Experiments on the horizon will reveal the nature of gravitational waves, dark matter, dark energy, and many other key questions of science: plenty of help needed! If this interests you: talk to teachers, scientists. Get an internship: do interesting things and meet fascinating people. Take college ...
... Experiments on the horizon will reveal the nature of gravitational waves, dark matter, dark energy, and many other key questions of science: plenty of help needed! If this interests you: talk to teachers, scientists. Get an internship: do interesting things and meet fascinating people. Take college ...
gwpaw - DCC
... Statistic for Combination of Results from Multiple Gravitational-Wave Searches Chris Pankow and Sergey Klimenko GWPAW 2011 Milwaukee, Wisconsin LIGO G1001168-v5 ...
... Statistic for Combination of Results from Multiple Gravitational-Wave Searches Chris Pankow and Sergey Klimenko GWPAW 2011 Milwaukee, Wisconsin LIGO G1001168-v5 ...
No Slide Title - DCC
... – #1 (314 mm x 130 mm): 60 ppm/cm average, 30 –130 ppm/cm range – #2 (314 mm x 130 mm): 31 ppm/cm average, 10 – 53 ppm/cm range – #3 (250 mm x 100 mm): 49-55 ppm/cm average, 29 –110 ppm/cm range ...
... – #1 (314 mm x 130 mm): 60 ppm/cm average, 30 –130 ppm/cm range – #2 (314 mm x 130 mm): 31 ppm/cm average, 10 – 53 ppm/cm range – #3 (250 mm x 100 mm): 49-55 ppm/cm average, 29 –110 ppm/cm range ...
Testing the black hole no-hair theorem using LIGO extreme mass
... • It is remarkable that the equations of motion separate for geodesic motion in the Kerr spacetime, giving a third integral, the Carter constant. Very surprising if this generalised. • Most orbits in most ‘quasi-Kerr’ spacetimes possess a third integral. Deviations only show up in precession and ins ...
... • It is remarkable that the equations of motion separate for geodesic motion in the Kerr spacetime, giving a third integral, the Carter constant. Very surprising if this generalised. • Most orbits in most ‘quasi-Kerr’ spacetimes possess a third integral. Deviations only show up in precession and ins ...
SOW- Trillium T-240 OBS Seismometers - DCC
... For the above list the Supplier shall: 1) Identify the corresponding sections/paragraphs in their existing QA/QC system 2) meet or exceed the design requirements contained in the attached engineering documents for each area called out. LIGO prefers to utilize the vendors existing QA/QC programs to t ...
... For the above list the Supplier shall: 1) Identify the corresponding sections/paragraphs in their existing QA/QC system 2) meet or exceed the design requirements contained in the attached engineering documents for each area called out. LIGO prefers to utilize the vendors existing QA/QC programs to t ...
SWFAS Mar 16 Newsletter - Southwest Florida Astronomical Society
... spacecraft to traverse the asteroid belt. Photography of Jupiter began November 6, 1973, at a range of 25,000,000 kilometers (16,000,000 mi), and a total of about 500 images were transmitted. The closest approach to the planet was on December 4, 1973, at a range of 132,252 kilometers (82,178 mi). Du ...
... spacecraft to traverse the asteroid belt. Photography of Jupiter began November 6, 1973, at a range of 25,000,000 kilometers (16,000,000 mi), and a total of about 500 images were transmitted. The closest approach to the planet was on December 4, 1973, at a range of 132,252 kilometers (82,178 mi). Du ...
PH507lecnote07_mcp5
... conjunction with four other gravitational wave detectors located in Italy, Japan and the United States. The U.S. detector, LIGO (Laser Interferometer Gravitational wave Observatory), is run by the California Institute of Technology and Massachusetts Institute of Technology and consists of two sites ...
... conjunction with four other gravitational wave detectors located in Italy, Japan and the United States. The U.S. detector, LIGO (Laser Interferometer Gravitational wave Observatory), is run by the California Institute of Technology and Massachusetts Institute of Technology and consists of two sites ...
G040471-01 - DCC
... System testing Initial LIGO experience: thorough testing offsite necessary Very significant feature in R&D plan: testing of accurate prototypes in context Two major facilities: » MIT LASTI facility – full scale tests of seismic isolation, suspensions, laser, mode Cleaner – 2004: pre-isolator ...
... System testing Initial LIGO experience: thorough testing offsite necessary Very significant feature in R&D plan: testing of accurate prototypes in context Two major facilities: » MIT LASTI facility – full scale tests of seismic isolation, suspensions, laser, mode Cleaner – 2004: pre-isolator ...
ppt source - LIGO dcc - LIGO Scientific Collaboration
... Limit on GW background from early universe Limits on GW waves emitted by GRBs and SGRs Limits on rates of mergers of black holes and neutron stars Determined that the short GRB 070201, possibly in M31, was either a compact binary merger at much greater distance or a different source in M31, such as ...
... Limit on GW background from early universe Limits on GW waves emitted by GRBs and SGRs Limits on rates of mergers of black holes and neutron stars Determined that the short GRB 070201, possibly in M31, was either a compact binary merger at much greater distance or a different source in M31, such as ...
IndIGO Indian Initiative in Gravitational
... (Beverly Berger, National Science Foundation Program director for gravitational physics. ) We already have a community of distinguished gravitational physicists/ astronomers in India ….. We are also lucky in having developed in several of our scientific institutes, the essential technical expertise ...
... (Beverly Berger, National Science Foundation Program director for gravitational physics. ) We already have a community of distinguished gravitational physicists/ astronomers in India ….. We are also lucky in having developed in several of our scientific institutes, the essential technical expertise ...
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.