Bulletin of the American Physical Society
APS April Meeting 2015
Volume 60, Number 4
Saturday–Tuesday, April 11–14, 2015; Baltimore, Maryland
Session J13: Focus Session: Beller Lectureship on Ground Based Gravitational Wave Detection |
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Sponsoring Units: GGR Chair: Ben Farr, Princeton University Room: Key 9 |
Sunday, April 12, 2015 10:45AM - 11:21AM |
J13.00001: LIGO-India: expanding the international network of gravitational wave detectors Invited Speaker: Balasubramanian Iyer The first detection of Gravitational Waves (GW) by ground based detectors will open up a fundamentally new observational window to the Universe with implications for astrophysics and eventually cosmology and fundamental physics. The realization of GW astronomy requires a global network of Advanced GW detectors including upcoming observatories like KAGRA (Japan) and LIGO-India to provide good sky localization of the GW sources. LIGO-India is expected to play a key role in locating and deciphering the sources contributing to the GW symphony. The current status of LIGO-India project and the exciting future research opportunities of this ambitious Indo-US collaboration in science, technology and computation will be finally indicated. [Preview Abstract] |
Sunday, April 12, 2015 11:21AM - 11:33AM |
J13.00002: Improvement of the GEO600 gravitational wave detector using squeezed states of light Katherine Dooley During the last 3 years, the GEO600 laser interferometer gravitational wave (GW) observatory, located near Hannover, Germany, has conducted the first long-term study of the permanent integration of a squeezed light source to such a detector. Squeezed vacuum states, which are generated using quantum optics, are injected into the output port of the laser interferometer, where they join the GW signal and improve the shot-noise-limited signal-to-noise ratio. An improvement up to a factor 1.5 above 800 Hz has been achieved at GEO600, as well as a squeezing application duty cycle of about $90\%$. New control loops have also been developed to ensure long-term stability of the integration of the squeezed light source to the GW detector. I will describe the squeezing experiment at GEO600 and report on the lessons learned for integration of a squeezed light source to future GW detectors, such as Advanced LIGO. [Preview Abstract] |
Sunday, April 12, 2015 11:33AM - 11:45AM |
J13.00003: Frequency dependent squeezed light at audio frequencies John Miller Following successful implementation in the previous generation of instruments, squeezed states of light represent a proven technology for the reduction of quantum noise in ground-based interferometric gravitational-wave detectors. As a result of lower noise and increased circulating power, the current generation of detectors places one further demand on this technique -- that the orientation of the squeezed ellipse be rotated as function of frequency. This extension allows previously negligible quantum radiation pressure noise to be mitigated in addition to quantum shot noise. I will present the results of an experiment which performs the appropriate rotation by reflecting the squeezed state from a detuned high-finesse optical cavity, demonstrating frequency dependent squeezing at audio frequencies for the first time and paving the way for broadband quantum noise reduction in Advanced LIGO. Further, I will indicate how a realistic implementation of this approach will impact Advanced LIGO both alone and in combination with other potential upgrades. [Preview Abstract] |
Sunday, April 12, 2015 11:45AM - 11:57AM |
J13.00004: Experimental Limits on Gravitational Waves in the MHz Frequency Range with the Fermilab Holometer Robert Lanza We present the results of a search for gravitational waves in the 1-10MHz frequency range using dual power-recycled Michelson laser interferometers at Fermi National Accelerator Laboratory. An unprecedented level of sensitivity to gravitational waves in this frequency range has been achieved by cross-correlating the output fluctuations of two identical and co-located 40m long interferometers. This technique produces sensitivities better than two orders of magnitude below the quantum shot-noise limit, within integration times of less than 1 hour. Limits are placed on the strain amplitude of MHz frequency gravitational waves at the $10^{-21} \mathrm{Hz}^{-1/2}$ level, constituting the best direct limits to date at these frequencies. In this talk, I will discuss the detector technology, the data analysis, and the gravitational wave limit results. [Preview Abstract] |
Sunday, April 12, 2015 11:57AM - 12:09PM |
J13.00005: Optical Coating Thermal Noise Testbed Michael T. Hartman, Johannes Eichholz, David B. Tanner, Guido Mueller Interferometric gravitational-wave detectors measure the length strain of a passing gravitational-wave as differential arm length changes in kilometer-long Michelson interferometers. The second-generation detectors, such as Advanced LIGO (aLIGO), will achieve strain sensitivities which are limited by Brownian thermal noise in the optical coatings of the interferometers' arm-cavity mirror test masses. Brownian coating thermal noise (CTN) is the apparent motion on the mirror surface on the order of $10^{-17} - 10^{-20}\,\mathrm{m}$ resulting from thermal fluctuations in the coating and the coating's internal friction. The result is a source of length noise in optical resonators that is a function of the coating temperature and the coating material's mechanical loss. At the University of Florida we are constructing the THermal noise Optical Resonator (THOR), a testbed for the direct measurement of CTN in the aLIGO test mass coating as well as future coating candidates. The material properties of the coating (namely mechanical loss) are temperature dependent, making cryogenic mirrors a prospect for future gravitational-wave detectors. To explore this option we are simultaneously building a cryogenic CTN testbed, CryoTHOR. This is a presentation on the status of these testbeds. [Preview Abstract] |
Sunday, April 12, 2015 12:09PM - 12:21PM |
J13.00006: Progress towards the measurement of quantum radiation pressure noise Jonathan Cripe, Robinjeet Singh, Warren Johnson, Garrett Cole, Thomas Corbitt Advanced LIGO is predicted to be limited by quantum noise at intermediate and high frequencies when it reaches design sensitivity. The quantum noise, including radiation pressure noise at intermediate frequencies, will need to be reduced in order to increase the sensitivity of future gravitational wave interferometers. We report recent progress towards measuring quantum radiation pressure noise in a cryogenic optomechanical cavity. The low noise microfabricated mechanical oscillator and cryogenic apparatus allow direct broadband thermal noise measurements which test thermal noise models and damping mechanisms. We also present plans for the measurement of the ponderomotive squeezing produced by the optomechanical cavity and the reduction of radiation pressure noise. These techniques may be applicable to an upgrade of Advanced LIGO or the next generation of gravitational wave detectors. [Preview Abstract] |
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