Bulletin of the American Physical Society
2005 72nd Annual Meeting of the Southeastern Section of the APS
Thursday–Saturday, November 10–12, 2005; Gainesville, FL
Session BB: Gravitational Wave Detection |
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Chair: Guido Mueller, University of Florida Room: Hilton Hawthorne |
Thursday, November 10, 2005 8:30AM - 8:42AM |
BB.00001: Calculating gravitational waveforms for LISA Steven Detweiler A small, solar mass object orbiting a jumbo sized black hole emits gravitational waves which might be in the LISA bandwidth. Relativists have an obligation to provide accurate calculations of the possible waveforms. These calculations involve a number of subtle issues which are of fundamental as well as practical interest. [Preview Abstract] |
Thursday, November 10, 2005 8:42AM - 8:54AM |
BB.00002: Experimental Verification of Arm Locking for LISA James Ira Thorpe, Shawn Mitryk, Guido Mueller The Laser Interferometer Space Antenna (LISA) is a joint effort of NASA and ESA to build a space-based gravitational wave detector which will study gravitational waves in the 10-4 Hz to 10-1 Hz frequency regime. The mission calls for a constellation of three separate spacecraft (SC) flying in a triangular formation with an intra-SC distance of 5 Gm. The distance between the SC will be measured interferometrically with pm accuracy in an effort to detect modulations caused by gravitational waves. A major challenge for these measurements is reducing the phase noise of the laser light source. A technique known as arm-locking has been proposed to address this problem. We present the results of arm-locking in an electronic model of LISA. Additionally, we discuss progress towards integrating the electronic model with an optical model of the LISA interferometry. This combined model will incorporate many of the essential features of the LISA interferometry and will allow us to test arm-locking under more realistic conditions. [Preview Abstract] |
Thursday, November 10, 2005 8:54AM - 9:06AM |
BB.00003: Measurement of residual amplitude modulation in the electro-optic modulator for Advanced LIGO Wan Wu, Guido Mueller, David Reitze, David Tanner The Laser Interferometer Gravitational Wave Observatory (LIGO) is designed to measure the infinitesimal distortions of space created by the motion of massive astronomical bodies. The interferometer consists of several Fabry-Perot cavities which are sensed and controlled with extremely high precision using heterodyne methods based on the Pound-Drever-Hall scheme. An electro-optic modulator (EOM) is a key component for the implementation of these shemes. The residual amplitude modulation produced by the phase modulator can produce a DC signal detected at the antisymmetric port of the LIGO interferometer. It is indistinguishable from the signature of the arm cavity length. The limitation on the arm length difference thus put an upper limit on the fractional field amplitude modulation. I will talk about the experiment to measure the amplitude modulation of the new 180 MHz resonant circuit modulator that was propsed to be used for the Advanced LIGO, the upgraded version of LIGO. [Preview Abstract] |
Thursday, November 10, 2005 9:06AM - 9:18AM |
BB.00004: Near-field Radiative Coupling for Low-Temperature Gravitational Wave Detectors Stacy Wise, V. Quetschke, D.B. Tanner, B.F. Whiting Future interferometric gravitational-wave detectors will likely be cooled to cryogenic temperatures to produce unprecedented sensitivities. Mirrors serve as test masses for detection of gravitational wave response in instruments such as LIGO, and their internal thermal noise must not prevent measurements from reaching the quantum limit determined by the circulating light power in the interferometer. In order to maintain isolation of the mirrors from ground noise, the cooling should be achieved without physically touching the test masses. Although ordinary thermal radiative emission (Stefan-Boltzmann radiation) is inadequate, if a cold object were brought close enough to the test mass to allow significant electromagnetic coupling via evanescent fields, the heat transfer can increase by several orders of magnitude. The very fact that the cold mass and test mass are coupled creates a path for the introduction of noise mirror motion, and this is also analyzed. [Preview Abstract] |
Thursday, November 10, 2005 9:18AM - 9:30AM |
BB.00005: Implementation of Time Delay Interferometry using the UF LISA simulator Rachel J. Cruz, Michael Hartman, Guido Mueller The Laser Interferometer Space Antenna (LISA) is a joint mission between NASA and ESA to detect gravitational waves generated by astronomical sources in the range of 0.1 mHz to 0.1 Hz. LISA is comprised of three spacecraft separated by five million kilometers in a triangular formation. In order to detect gravitational waves, LISA must measure differences between the spacecraft to an accuracy of picometers per square root Hertz. Due to the orbits of the spacecraft, the distances of the interferometer arms will not be equal. This arm mismatch results in laser frequency noise being the dominant noise source. The interferometric measurement can be brought below detection requirements by using a method called time delay interferometry (TDI) which cancels the laser frequency noise. We will test the implementation of first-generation TDI in an optical system using the LISA simulator that is being developed at the University of Florida. I will present the current status of the frequency stabilization and cancellation experiment in the LISA simulator. [Preview Abstract] |
Thursday, November 10, 2005 9:30AM - 9:42AM |
BB.00006: Search for gravitational waves with LIGO. Sergey Klimenko The Laser Interferometer Gravitational-Wave Observatory (LIGO) is a facility at US dedicated to the detection of cosmic gravitational waves. It consists of three detectors operated in unison as a single observatory. The LIGO observatory is a part of a developing global network of gravitational wave detectors. I will talk about recent LIGO results and future prospects. [Preview Abstract] |
Thursday, November 10, 2005 9:42AM - 9:54AM |
BB.00007: Low absorption thermally adjustable telescope J. Gleason, V. Quetschke, M. Rakhmanov, J. Lee, G. Mueller, D.H. Reitze, D.B. Tanner In the advancing field of gravitational wave interferometry, the desire for greater sensitivity leads to higher laser powers to reduce shot noise. One of the major challenges in using higher power lasers is the creation of thermal lenses in optical components. This is especially problematic in transmissive optical components even at very low levels of absorbed power. Using an additional laser with a wavelength heavily absorbed by the substrate, an aberration-free parabolic lens can be created. We present experimental and theoretical results on thermally adjustable lenses using fused silica as a substrate material with very low absorption for the 1064nm wavelength Nd:YAG lasers that are used for GW detectors. We characterize the dynamical focal range of the system, measure the resulting aberrations on the transmitted Nd:YAG beam and use this lens to mode match into an optical cavity. Our results are in good agreement with theoretical model incorporating the temperature distribution of the lens and the relevant thermo-optic parameters. [Preview Abstract] |
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