Bulletin of the American Physical Society
APS April Meeting 2022
Volume 67, Number 6
Saturday–Tuesday, April 9–12, 2022; New York
Session G15: Gravitational Wave Detection: Noise Modeling and MitigationRecordings Available
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Sponsoring Units: DGRAV Chair: Ling Sun, Australian National Univ Room: Marquis C |
Sunday, April 10, 2022 8:30AM - 8:42AM |
G15.00001: Characterization of gravitational-wave detector noise with fractals Marco Cavaglia Current ground-based gravitational-wave detectors such as the Laser Interferometer Gravitational-wave Observatory (LIGO), Virgo, and KAGRA, are exquisite scientific instruments of extreme sensitivity. Characterization of detector noise and data quality investigations are essential to improve the instruments, provide feedback to commissioners, as well as validate detection candidates in low-latency and increase the significance of gravitational-wave signals in searches. We present a new method, based on fractal analysis, to characterize the data of gravitational-wave interferometric detectors. We show that a measure of the fractal dimension of the main detector output (strain channel) can be used to determine the instrument state, test data stationarity, and identify non-astrophysical excess noise in low latency. When applied to instrument control and environmental data (auxiliary channels) the fractal dimension can be used to identify the origins of noise transients, non-linear couplings in the various detector subsystems, and provide a means to flag stretches of low-quality data. |
Sunday, April 10, 2022 8:42AM - 8:54AM |
G15.00002: Accurate modeling and mitigation of overlapping signals and glitches in gravitational wave data Sophie R Hourihane, Katerina Chatziioannou, Marcella Wijngaarden, Neil J Cornish, Tyson Littenberg Transient noise artifacts or “glitches” in LIGO detector data challenge parameter estimation of gravitational wave signals. We present a method that concurrently fits for glitches and gravitational waves by separating them into a template and a wavelet model. We show the efficacy of this method on black hole and neutron star binaries atop a range of glitch types. |
Sunday, April 10, 2022 8:54AM - 9:06AM |
G15.00003: Mitigating the effects of glitches on gravitational-wave event sky localizations Derek Davis, Maggie Huber Electromagnetic follow up of gravitational-wave signals relies on fast, accurate sky localizations based on gravitational-wave data. Transient instrumental artifacts, known as glitches, are present in the data and can coincidently overlap a transient gravitational-wave signal. If this occurs, then the estimated source sky location of the signal may be biased and prevent identification of an electromagnetic counterpart. Numerous methods have been developed to subtract the glitch noise from data, but are either not quick enough to be used in low latency or introduce their own biases. In this talk, we demonstrate how inpainting techniques can be used to remove glitches that overlap gravitational-wave signals from compact binary mergers. We then present a method to account for the impact of the data that was removed and calculate new bias-free sky localizations in only a few seconds. Only knowledge of the time and duration of a glitch is required to calculate a new sky localization, allowing this method to be used for a wide array of different artifacts. We further show how this method can also be used to test if the estimated source sky location was biased before this method was applied. |
Sunday, April 10, 2022 9:06AM - 9:18AM |
G15.00004: Noise Transients in the LIGO Livingston Detector Due to Trains Jane Glanzer, Gabriela Gonzalez One of the many types of transient noise observed in the Advanced LIGO gravitational wave detectors is due to light scattered from surfaces with large relative motion. These transients increase the background noise for astrophysical searches and reduces the reach of the detectors. This noise caused by low frequency anthropogenic and microseismic motion can be identified as small duration arches in time-frequency space in the main gravitational wave data channel. Trains near the LIGO Livingston (LLO) Y end station are one of the main causes of increased ground motion in the anthropogenic frequency range. In this presentation we investigate the noise caused by trains. Specifically, we investigate trains that happened during O3 and their corresponding detector glitches. Preliminary results identify 583 trains and 8051 glitches due to these trains in O3. To help find the location of the surfaces that produce the scattering noise, we look for correlations between the glitches and ground motion due to trains in both the LLO Y end station, and in the corner station. |
Sunday, April 10, 2022 9:18AM - 9:30AM |
G15.00005: Alignment and Transient Noise Reduction in aLIGO Shania A Nichols After a very successful third observation run, the aLIGO detectors are undergoing upgrades in preparation for the fourth observation run. Alignment noise is one of the largest contributors of noise at low frequency in the detection bandwidth. The mirrors of the detector are actively aligned to maintain resonance in the optical cavities. In this talk I will discuss the ongoing effort to reduce this alignment noise. I will also present about transient noise and its possible links to the alignment control loops. |
Sunday, April 10, 2022 9:30AM - 9:42AM |
G15.00006: Impact of calibration uncertainties on Hubble constant measurements from gravitational-wave sources Yiwen Huang, Hsin-Yu Chen, Carl-Johan O Haster, Ling Sun, Salvatore Vitale, Jeffrey S Kissel Gravitational-wave detections of electromagnetically bright compact binary coalescences can provide an independent measurement of the Hubble constant $H_0$ with the standard siren method. In order to obtain a measurement that could help arbitrating the existing tension on $H_0$, one needs to fully understand any source of systematic biases for this approach. In this talk, we present results for our study that investigates the impact of instrumental calibration errors on the inferred Hubble constant results. We simulate binary neutron star mergers detected by the network of Advanced LIGO and Advanced Virgo interferometers at their design sensitivities. We artificially add exceptionally large calibration errors as experienced in LIGO-Virgo's third observing run, and we will present the $H_0$ measurements after combining multiple events. |
Sunday, April 10, 2022 9:42AM - 9:54AM |
G15.00007: Exposing gravitational-wave signals below the shot noise with quantum correlation Hang Yu, Denis Martynov, rana X adhikari, Yanbei Chen The sensitivities of ground-based gravitational wave (GW) detectors are limited by quantum shot noise at > a few x 100 Hz. Nonetheless, one can use a quantum correlation (QC) technique to remove the expectation value of the shot noise, thereby exposing underlying classical signals in the cross spectrum form by cross-correlating two photodiodes in a GW detector's antisymmetric port. The QC technique has been used to constrain the coating thermal noise in LIGO. Here we further explore the prospects and analyze the sensitivity of using the QC to detect GW signals, including both bursts with short and long durations and persistent GW emissions from pulsars with unknown locations. While conceptually similar to the correlation of two different interferometers, the QC has its unique advantages. In particular, with GC one can detect signals with only a single interferometer. Therefore, the QC technique does not require corrections to the differences in a signal's arrival time and antenna response which are necessary when cross-correlating two different detectors. This makes the QC computationally efficient when searching for sources with unknown locations. |
Sunday, April 10, 2022 9:54AM - 10:06AM |
G15.00008: Gravitational Wave Observartions In Non-Stationary Detector Noise Neil J Cornish As ground based interferometers continue to improve in sensitivity, especially at low frequencies, and with the advent of future space based interferometers, the duration that gravitational wave signals spend in the sensitive band of the detectors will increase. The assumption that the noise can be treated as approximately stationary breaks down for these long duration signals, and analyses that assume stationarity will produce biased results. The biases can be removed by properly modeling the non-stationary behaviour using wavelet domain, time-frequency modeling of the data and signals. |
Sunday, April 10, 2022 10:06AM - 10:18AM |
G15.00009: Noise budget for the NANOGrav pulsar timing array Jeffrey S Hazboun, Xavier Siemens, Michael T Lam The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) recently reported on the presence of a time-correlated stochastic signal across the pulsars in our 12.5-year dataset. While we detect a common spectral process consistent with that expected from supermassive binary black holes, spatial correlations (Hellings-Downs correlations) between the pulsars have not been detected and are necessary in order to claim detection of a gravitational wave background (GWB). As NANOGrav prepares for a GWB search in the 15-year dataset we have undertaken a full accounting of the noise in individual pulsars. The standard noise model in our pulsars consists of a white noise model together with a power-law red noise model, i.e., time-correlated noise with more power in lower frequencies. This full noise budget of our phenomenological model compares the noise power spectral density in our noise models to the spectral characteristics of the common spectral process detected in the NANOGrav 12.5-year analysis. |
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