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  • Graduate Research at Caltech in Experimental Gravitational Physics
    collision and coalescence of two neutron stars or black holes that are orbiting each other the rotation of neutron stars with deformed crusts star quakes in neutron star crusts and the big bang origin of the universe A gravitational wave is a perturbation in the curvature of space time that travels at the speed of light As it passes it causes adjacent inertial frames and free masses carried along by those frames to move relative to one another A gravitational wave can be detected by carefully monitoring the resulting fluctuations ΔL in the separation L between two free masses The ratio ΔL L is directly proportional to the wave s amplitude thus large separations L result in detectable fluctuations ΔL The strongest sources e g black hole collisions and supernova explosions are likely to cause fluctuations of magnitude ΔL L 10 21 between free masses on earth LIGO Hanford Observatory In the LIGO these small relative displacements ΔL are measured using laser interferometry Each interferometer has four mirrored test masses arranged in pairs to form two long L 4 km resonant optical cavities situated at right angles to each other forming a Michelson interferometer LIGO operates three such interferometer detectors located at two widely separated sites in the United States two in Hanford Washington and one in Livingston Parish Louisiana operated in coincidence for the detection of gravitational waves By making high precision measurements over such long baselines LIGO interferometers will be able to see gravitational radiation originating from distant sources in the universe Compared to laboratory scale apparatus this should make the difference between detecting a few events per century and detecting several per year Because the LIGO detectors will operate over a broad band of frequencies from 10 Hz to 10 kHz they should be able not only to detect a gravitational wave but also to reveal the details of the wave s time evolution i e of its waveform From the waveform it will be possible to infer the details of the dynamical evolution of the waves source that will rarely be obtainable from electromagnetic waves since most gravitational wave sources are likely to be surrounded by dense layers of matter e g the core of a supernova or the big bang or to be made of pure gravity which emits no electromagnetic waves e g colliding black holes LIGO Livingston Observatory The three Initial LIGO detectors have achieved noise limited strain sensitivity consistent with their design and are taking data in a series of science runs The current science run S5 extends through 2007 and analysis of the data to search for gravitational wave signals is underway The LIGO Laboratory plans to implement a modest upgrade Enhanced LIGO to improve the sensitivity by a factor 2 3 and then take date through 2011 Plans for Advanced LIGO interferometers with an order of magnitude improved sensitivity resulting in a thousand fold increase in event rate are well under way for installation in 2011 2013 These upgrades hold

    Original URL path: http://www.ligo.caltech.edu/LIGO_web/students/grads.html (2015-06-02)
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  • Undergraduate Research at LIGO
    The Undergraduate SURF page has moved You will be redirected in 1 second If you are not redirected automatically follow this link to the new SURF page

    Original URL path: http://www.ligo.caltech.edu/LIGO_web/students/undergrads.html (2015-06-02)
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  • LIGO Core Optics Components
    H1 2005 Advanced LIGO COC LIGO 40M RSE COC Gingin Shortcuts to Optic Index Status links also available from project pages LIGO1 COC Pathfinder and links to explicit data 40 Meter RSE Advanced LIGO R D substrates Lasers and Optics

    Original URL path: http://www.ligo.caltech.edu/~gari/ (2015-06-02)
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  • Advanced LIGO
    The Advanced LIGO page has moved If the browser does not automatically redirect you please follow this link http www advancedligo mit edu

    Original URL path: http://www.ligo.caltech.edu/advLIGO/ (2015-06-02)
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  • LIGO Sensitivities Home Page
    This web site has been moved please change any bookmarks you may have to The new LIGO Sensitivities Home Page

    Original URL path: http://www.ligo.caltech.edu/~lazz/distribution/LSC_Data/ (2015-06-02)
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  • Data Monitor Tool Project
    is some introductory material for beginning users with a primary focus on High Energy Physics analysis The Sandbox library contains C classes and functions ROOT Macros which support interactive monitoring and fault diagnosis It includes an online data interface and signal processing functions A Software Distribution Kit containing the Sandbox software and useful utility functions may be downloaded from this site Examples of ROOT sessions using the Sandbox Background Environments

    Original URL path: http://www.ligo.caltech.edu/~jzweizig/dmt/DMTProject/ (2015-06-02)
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  • e2e home page
    e2e home page

    Original URL path: http://www.ligo.caltech.edu/~e2e/ (2015-06-02)
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  • LIGO General Computing Information
    on the LIGO network use good passwords and change them every 6 months What is a good password use different passwords for different accounts and locations contact the local system administrator for help with any questions or problems keep your computers and laptops in a secure location to prevent theft Do not share your password with others install pirated software or products not licensed for use by LIGO including personal

    Original URL path: http://www.ligo.caltech.edu/LIGO_web/GC/comp_abbr.shtml (2015-06-02)
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