Bulletin of the American Physical Society
APS April Meeting 2019
Volume 64, Number 3
Saturday–Tuesday, April 13–16, 2019; Denver, Colorado
Session R11: Improving LIGO and Other High-Frequency Gravitational-Wave Detectors |
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Sponsoring Units: DGRAV Chair: Evan Hall, Massachusetts Institute of Technology Room: Sheraton Governor's Square 17 |
Monday, April 15, 2019 1:30PM - 1:42PM |
R11.00001: Reducing technical noise in Advanced LIGO Detectors Corey Austin Since the second LIGO observing run ended in August 2017, several upgrades have been made to the detectors to limit noise from technical sources in order to improve instrument sensitivity. This talk will describe the efforts towards reducing the noise introduced by scattered light, reducing the coupling of stray electric fields to the interferometer, and improving duty cycle by adding ground rotation sensors to the seismic isolation system. |
Monday, April 15, 2019 1:42PM - 1:54PM |
R11.00002: Reducing Quantum Noise in Advanced LIGO detectors Terra Hardwick During the first two observing runs, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected gravitational waves from the merging of multiple binary black hole systems and one binary neutron star system. Following a period of down time for upgrades, LIGO's third observing run will begin early 2019 and continue for approximately one year. Upgrades include increased laser input power and squeezed quantum state injection to reduce fundamental quantum noise. This talk discusses these upgrades and their impact on our sensitivity. |
Monday, April 15, 2019 1:54PM - 2:06PM |
R11.00003: How to Study LIGO Noise Beverly K. Berger In order to increase the sensitivity of Advanced LIGO to astrophysical events, various sources of instrumental and environmental noise must be identified and ameliorated. Here we explore a single example from the LIGO Hanford instrument. On April 10, 2017, a cluster of strong glitches (transient noise events) were clearly visible in the gravitational wave channel between 16:30 and 18:30 UTC. LIGO Scientific Collaboration scientists have developed software tools to search for correlations between anomalous behavior in the gravitational wave channel and the performance recorded by the myriad of instrumental or environmental sensors operating at that time. We will show how these tools are used to identify possible causes for the observed glitches. |
Monday, April 15, 2019 2:06PM - 2:18PM |
R11.00004: Numerically calculating the thermal noise of mirror coatings with multiple loss angles Samuel Rodriguez, Geoffrey Lovelace Reducing Brownian coating thermal noise is crucial for increasing the sensitivity of ground-based gravitational-wave detectors. One promising idea to decrease thermal noise is to use crystalline coatings. Modeling thermal noise from crystalline coatings is technically challenging. In this talk, I will discuss new numerical calculations that model Brownian coating thermal noise for crystalline coatings using the fluctuation-dissipation theorem. For simplicity, such calculations often approximate materials as having a single loss angle (loss angles, resulting from small imaginary parts of materials' elastic moduli, lead to dissipation). In this talk, I will present results that include different loss angles for different elastic moduli, and I will compare them to results using a single loss angle. |
Monday, April 15, 2019 2:18PM - 2:30PM |
R11.00005: Complex modulation for Advanced LIGO Hanyu Chia, Alexander Schindler-Tyka, John Conklin, Guido Mueller, David Burnham Tanner Multistage optical phase modulation is used to control the interferometer length and alignment degrees of freedom in Advanced LIGO, VIRGO, and KAGRA. Phase modulation of the laser at RF frequency Ω produces sidebands at ω ± Ω, where ω is the laser frequency (the "carrier"). To achieve multiple modulation frequencies, multiple electro-optic modulators (EOMs) are used in series. The second and following EOMs impose sidebands not only on the carrier but on the sidebands produced by the upstream EOMs. This problem, called “sidebands on sidebands,” can affect the extraction of the interferometer control signals. A method of addressing it is called “complex modulation.” Complex modulation requires specific functions—produced by arbitrary-function generators—to be applied simultaneously to amplitude and phase modulators. The modulating functions are calculated to produce the desired modulation pattern on the laser. Two practical applications have been studied: single-sideband modulation and suppression of sidebands on sidebands. The results have been analyzed and compared to simulations. We also conducted characterization of practical modulators in an effort to understand the setup better and to provide accurate inputs for simulations. |
Monday, April 15, 2019 2:30PM - 2:42PM |
R11.00006: Can we cloak LIGO from Seismic Waves? Brittany Kamai Advances in seismic cloaking design and experimentation offer intriguing applications to fundamental physics experiments. Achieving full implementation of a seismic cloak will mean that precious infrastructure is shielded from seismic waves. The key is to design seismic meta-materials, which are a people-designed configuration of a 'material' that will attenuate and redirect the waves. Recent experiments on seismic meta-materials at low frequencies have proven that attenuation is in fact possible. In thinking about next generation seismic isolation for LIGO, seismic meta-materials offer a potential pathway. In this talk, I will discuss the connection between seismic meta-material design and the impact on LIGO sensitivity. |
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