Bulletin of the American Physical Society
APS April Meeting 2020
Volume 65, Number 2
Saturday–Tuesday, April 18–21, 2020; Washington D.C.
Session D05: Improving the Sensitivity of LIGO and Future Ground-Based Gravitational Wave DetectorsLive
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Sponsoring Units: DGRAV Chair: James Thorpe, NASA Goddard Space Flight Center Room: Washington 6 |
Saturday, April 18, 2020 3:30PM - 3:42PM Live |
D05.00001: Noise from thunderstorms coupling into the LIGO gravitational-wave observatory Guillermo Valdes, Ericka Florio, Brina Martinez, Erin Thompson, Anamaria Effler, Gabriela Gonzalez, Brian O'Reilly, Alexander Urban The observation of gravitational waves requires extremely sensitive detectors, such as LIGO and VIRGO. Its sensitivity can be overwhelmed by local environmental noises such as the ones produced by thunderstorms. We have developed a new tool to identify thunders using acoustic features extraction, machine learning algorithms, and multilateration and posteriorly quantify their effect on the LIGO Livingston observatory (LLO). We found that the LLO's detection range decreased by 10\% during thunderstorms and that there is a high correlation between the vibrations in one of the vacuum chambers and the noise between 20Hz and 50Hz in the gravitational-wave channel. [Preview Abstract] |
Saturday, April 18, 2020 3:42PM - 3:54PM Live |
D05.00002: Seismic Issues at LIGO Livingston Observatory (LLO) during the LIGO-Virgo 3rd Observing Run (O3) Beverly K. Berger The Advanced LIGO/Virgo era of discovery would not be possible without effective isolation from seismic disturbances. Yet, such systems are not perfect. Stray light from seismically induced scattering creates noise in the monitored gravitational-wave channel, $h(t)$, that can mimic, distort, or obscure astrophysical signals. External influences at LLO such as storms and logging create time, frequency, and location dependent seismic noise. The identification of various components of the seismic noise and their impact on $h(t)$ will be the focus of this talk. Software tools including the Summary Pages, hVeto, and Lasso can help connect seismic disturbances with anomalies in $h(t)$. The status of understanding and mitigating the seismic disturbances will be discussed. [Preview Abstract] |
Saturday, April 18, 2020 3:54PM - 4:06PM Live |
D05.00003: Measuring Nonequilibrium Thermal Noise Effects for Gravitational-Wave Detectors Jennifer Sanchez One of the most important noise sources for current and future gravitational-wave detectors is thermal noise. A standard way to measure thermal noise relies on the assumption that the system is in thermal equilibrium, however, most natural systems are not in thermal equilibrium. Since there is no complete theory that explains thermal noise in nonequilibrium states, experimental exploration is important for understanding how nonequilibrium effects might contribute to thermal noise, including thermal noise for gravitational-wave detectors. In this talk, I will describe an experiment whose aim is to explore nonequilibrium thermal noise. Using a mechanical resonator with low frequency acoustic modes placed in a vacuum chamber, we introduce a thermal gradient that allows us to observe how the transverse and longitudinal resonant modes behave and thus to determine the amplitude spectral density of the thermal noise. We tested this method on a resonator in thermal equilibrium, and the experiment with a resonator not in thermal equilibrium is ongoing. [Preview Abstract] |
Saturday, April 18, 2020 4:06PM - 4:18PM Live |
D05.00004: Measurements of Optical Scatter versus Annealing Temperature for Ta2O5 and Ti:Ta2O5 thin-film coatings Elenna Capote, Joshua Smith, Amy Gleckl, Jazlyn Guerrero, Erick Engelby, Michael Rezac Light scattered by amorphous thin-film optical coatings limits the sensitivity of interferometric gravitational-wave detectors. We describe an imaging scatterometer to assess the role that crystal formation and growth during annealing plays in this scatter. We present results of measuring scatter while annealing Ta2O5 and Ti:Ta2O5 thin-film coatings to high temperatures in vacuum. [Preview Abstract] |
Saturday, April 18, 2020 4:18PM - 4:30PM Live |
D05.00005: LIGO Voyager: A Cryogenic Silicon Interferometer for Gravitational-wave Detection Raymond Robie, Aidan Brooks, Christopher Wipf, Koji Arai, Rana Adhikari The detection of gravitational waves from compact binary mergers by LIGO has opened the era of gravitational wave astronomy, revealing a previously hidden side of the cosmos. To maximize the reach of the existing LIGO observatory facilities, we have designed a new instrument that will have 5 times the range of Advanced LIGO, or greater than 100 times the event rate. Observations with this new instrument will make possible dramatic steps toward understanding the physics of the nearby universe, as well as observing the universe out to cosmological distances by the detection of binary black hole coalescences. Implementation of this new instrument utilizes much of the current LIGO infrastructure, and there are no fundamental noise obstacles or unrealistic engineering requirements for its implementation. Thus, its commissioning and operation are feasible on a realistic timescale and budget. This presentation will highlight the design concept for this next generation ground based gravitational wave detector, focusing on the instrument hardware upgrades and a quantitative analysis of the anticipated noise floor. [Preview Abstract] |
Saturday, April 18, 2020 4:30PM - 4:42PM Live |
D05.00006: Cosmic Explorer: the proposed U.S. contribution to the third-generation gravitational-wave detector network. Joshua Smith Cosmic Explorer (CE) is a 40 km L-shaped ground-based gravitational-wave observatory concept envisioned to begin operations in the 2030s. It is designed to be built in two phases, the first using scaled up Advanced LIGO$+$ technology, and the second incorporating new technologies and cryogenic temperatures. With its spectacular sensitivity, CE will observe gravitational-wave sources across the history of the universe. Sources that are barely detectable by today's instruments will be resolved with incredible precision. [Preview Abstract] |
Saturday, April 18, 2020 4:42PM - 4:54PM Live |
D05.00007: Superconducting GW detectors targeting 10$^{\mathrm{-30}}$ Hz$^{\mathrm{-1/2}}$ strain sensitivity at 100 Hz Armen Gulian, Joe Foreman, Vahan Nikoghosyan, Louis Sica, Shmuel Nussinov, Jeff Tollaksen, Chris Burdette, Rajendra Dulal, Serafim Teknowijoyo, Sara Chahid A design of compact (\textless 100 m in size) orbital detector of gravitational wave (GW) radiation with sensitivity up to 10$^{\mathrm{-30}}$ /Hz$^{\mathrm{1/2}}$ at and below 100 Hz is reported. The detector is not interferometric and uses superconducting Cooper pairs in magnetic field as transducers of GW-induced mechanical motion into electric current. Compactness yields ability to aim these portable detectors toward the source of GW, maximizing signal output and determining the direction of the source with high accuracy. The main idea of this design exploits the fact that an incident GW shifts infinitesimally the orientation of a 3D-superconducting system relative to a magnetic field. This minute change of orientation breaks the inherent symmetry of the Meissner current flowing on the surface layers of the superconducting system, thus serving as a ``valve regulator'' for the Meissner current flow. As a result, a current strong enough to be detected by means of superconducting electronics is being generated by the GW action. The inherent quietness of superconducting state is complemented by additional means, such as digital noise cancellation using second immobile system and noise filtering. The whole system acts as an amplified source of the current which is proportional to the amplitude of GW, similar to LIGO. [Preview Abstract] |
Saturday, April 18, 2020 4:54PM - 5:06PM Not Participating |
D05.00008: Applications of complex modulation Hanyu Chia, Alexander Schindler-Tyka, Scott Aaronson, John Conklin, Paul Fulda, David B. Tanner Residual amplitude modulation (RAM) from a variety of sources is observed when using standard optical phase modulation. A consequence is undesired offset in optical cavity control signals, such as the optical cavities in Advanced LIGO. Here we present a study in which we simultaneously modulate the amplitude and the phase of a laser beam, an approach we call ``complex modulation'' (CM). CM provides a powerful method to reduce RAM. CM is also capable of generating designer modulation signals, such as single sideband (SSB) modulation and sideband-on-sideband suppression. All three applications of CM have been experimentally demonstrated. At least 10 dB of RAM reduction and 20 dB of second-order sideband suppression are observed. The experimental results were have been compared to detailed CM simulations. [Preview Abstract] |
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