Bulletin of the American Physical Society
APS April Meeting 2018
Volume 63, Number 4
Saturday–Tuesday, April 14–17, 2018; Columbus, Ohio
Session S14: Gravitational Waves: Detectors and Instrumentation |
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Sponsoring Units: DGRAV Chair: Jenne Driggers, California Institute of Technology Room: A226 |
Monday, April 16, 2018 1:30PM - 1:42PM |
S14.00001: Mitigation of the angular noise sources in Advanced LIGO Marie Kasprzack The remarkable sensitivities reached by the LIGO detectors during their successful second observing run are now under improvement to prepare for the third observing run starting this year. One of the main limits of the sensitivity in the low-frequency part of the detection bandwidth is the angular motion of the core optics. The cavities are actively aligned to maintain the angular motion at the design requirements. In this talk I will discuss the angular noise sources that affected the detectors during the second observing run and their mitigation. I will also present the challenges linked to the foreseen increase of power in the detectors and their effect on the interaction between the longitudinal and angular motions. [Preview Abstract] |
Monday, April 16, 2018 1:42PM - 1:54PM |
S14.00002: The A$+$ upgrade for Advanced LIGO Lisa Barsotti The Advanced LIGO gravitational wave detectors, together with Virgo, have recently completed their second observing run, O2, making several detections of gravitational waves from binary black holes, and the first from a binary neutron star system. As the detectors evolve to reach their design sensitivity, the LIGO gravitational wave community is working on a concept for a near term upgrade, called A$+$, to improve the sensitivity of Advanced LIGO by up to a factor of 2 beyond its design goal. In this talk I will present the A$+$ concept, focusing on some key technologies that will be employed, such as squeezed light. [Preview Abstract] |
Monday, April 16, 2018 1:54PM - 2:06PM |
S14.00003: Characterization of Advanced LIGO detectors to validate gravitational-wave signals Marissa Walker The Advanced LIGO gravitational-wave detectors recently completed an exciting second observing run, making several observations of binary black hole mergers and the first binary neutron star merger. We performed an extensive series of checks to characterize the detectors at the time of each detection, to determine (or rule out) the influence of instrumental and environmental noise on the signals. This talk will give an overview of the process of validating gravitational-wave events, including examples from detections made during the second observing run. [Preview Abstract] |
Monday, April 16, 2018 2:06PM - 2:18PM |
S14.00004: Tracking down the origins of Advanced LIGO noise: some examples Beverly K. Berger In order to increase the sensitivity of Advanced LIGO (aLIGO) to astrophysical events, various sources of instrumental and environmental noise must be identified and ameliorated. Here we provide examples of efforts to understand the origin of types of noise manifested as short-duration bursts (glitches) at LIGO Hanford Observatory (LHO). Among several examples of glitch classes found and understood at LHO in aLIGO's second observing run, O2, are glitches caused by airplanes, by an incorrect servo setting, and by thirsty ravens. For each class, the process of relating an observed anomaly in the gravitational wave channel to an instrumental or environmental cause will be described. [Preview Abstract] |
Monday, April 16, 2018 2:18PM - 2:30PM |
S14.00005: Identifying High Frequency noise using the Bilinear Coupling Veto Sudarshan Ghonge, Laura Cadonati, Nairwita Mazumder Short duration transients or glitches from terrestrial and instrumental sources can couple into the Laser Interferometer Gravitational-Wave Detector (LIGO). These glitches can potentially mimic Gravitational Waves (GW) from astrophysical sources and must be vetoed out. They are characterized by a central frequency which ranges from a few Hertz to several Kilohertz. The recent observation of GWs from the coalescence of a binary neutron star merger, GW170817 in the second observational run (O2) by LIGO, pushed the frequency range of interest to the high frequency region beyond 2 Kilohertz. To veto glitches in this range, we use the Bilinear Coupling Veto (BCV) pipeline. BCV helps determine correlations in a pair of glitches appearing in the noise channels x(t) and the gravitational wave strain channel h(t). Other veto techniques already in place infer correlations using statistical properties of the glitch pairs such as duration, central time etc. without actually dealing with the time series data. BCV is unique in that it calculates the linear correlation coefficient between the time series data representing the glitch pair. We present the status of tuning the BCV pipeline for data collected during O2. [Preview Abstract] |
Monday, April 16, 2018 2:30PM - 2:42PM |
S14.00006: Using Artificial Neural Networks for Glitch Identification in Advanced LIGO Donald Moffa, Kyle Rose, Les Wade, Maddie Wade In an effort to increase sensitivity and produce reliable sensitivity estimates in low-latency, the LIGO collaboration is beginning to incorporate machine learning algorithms into the process of vetting data for glitches. Glitches are transient noise instances that occur frequently in LIGO data. Machine learning algorithms could potentially be used to veto glitchy data in real time, which could improve the chance of confidently detecting gravitational waves with associated electromagnetic counterparts. In this work, we studied the effectiveness of Google's artificial neural network software package, Tensor Flow, for identifying unclean data segments. Tensor Flow, as implemented, had comparable effectiveness to other machine learning algorithms but showed more robustness to increased feature sets. [Preview Abstract] |
Monday, April 16, 2018 2:42PM - 2:54PM |
S14.00007: Abstract Withdrawn
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Monday, April 16, 2018 2:54PM - 3:06PM |
S14.00008: Denoising Gravitational Waves using Deep Learning with Recurrent Denoising Autoencoders Hongyu Shen, Zhizhen Zhao, Daniel George, Eliu Huerta Gravitational wave astronomy is one of the most rapidly growing fields of modern astrophysics, with observations being made frequently by the LIGO detectors. Gravitational wave signals are often extremely weak and the data from the detectors, such as LIGO, is contaminated with high levels of non-Gaussian and non-stationary noise, often containing transient disturbances which can obscure real signals. Traditional denoising methods, such as principal component analysis and dictionary learning, are not optimal for dealing with this non-Gaussian noise, especially for low signal-to-noise ratio gravitational wave signals. Furthermore, these methods are computationally expensive on large datasets. To overcome these issues, we introduce SMTDAE, a denoising autoencoder based on sequence-to-sequence bidirectional Long-Short-Term-Memory recurrent neural networks. We demonstrate the advantages of using our unsupervised deep learning approach and show that, after training only using simulated Gaussian noise, SMTDAE achieves superior recovery performance for gravitational wave signals embedded in real non-Gaussian LIGO noise. [Preview Abstract] |
Monday, April 16, 2018 3:06PM - 3:18PM |
S14.00009: UV-LED based charge control for LISA Taiwo Olatunde, Stephen Apple, Andrew Chilton, Samantha Parry, Peter Wass, Guido Mueller, John Conklin The residual test mass acceleration in LISA must be below 3 fm/s2/$\surd $Hz at all frequencies between 0.1 and 3 mHz. Test mass charge coupled with stray electrical potentials and external electromagnetic fields is a well-known source of acceleration noise. LISA Pathfinder uses Hg lamps emitting mostly around 254 nm to discharge the test masses via photoemission, but a future LISA mission launched around 2030 will likely replace the lamps with newer UV LEDs which have lower mass, better power efficiency, smaller size and higher bandwidth. This presentation will discuss charge control demonstrated on the torsion pendulum in AC and DC modes at the University of Florida using latest generation UV LEDs producing light at 240 nm with energy above the work function of pure Au. Results of Au quantum efficiency measurements (number of emitted electrons per incident photons) which is critical for bi-polar charge control will also be presented. [Preview Abstract] |
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