Bulletin of the American Physical Society
APS April Meeting 2016
Volume 61, Number 6
Saturday–Tuesday, April 16–19, 2016; Salt Lake City, Utah
Session U14: Advanced LIGO Methods and Results IV |
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Sponsoring Units: GGR Chair: Jessica McIver, LIGO Laboratory Room: 251AB |
Monday, April 18, 2016 3:30PM - 3:42PM |
U14.00001: Reconstructing gravitational wave source parameters via direct comparisons to numerical relativity I: Method Jacob Lange, Richard O'Shaughnessy, James Healy, Carlos Lousto, Deirdre Shoemaker, Geoffrey Lovelace, Mark Scheel, Serguei Ossokine In this talk, we describe a procedure to reconstruct the parameters of sufficiently massive coalescing compact binaries via direct comparison with numerical relativity simulations. For sufficiently massive sources, existing numerical relativity simulations are long enough to cover the observationally accessible part of the signal. Due to the signal's brevity, the posterior parameter distribution it implies is broad, simple, and easily reconstructed from information gained by comparing to only the sparse sample of existing numerical relativity simulations. We describe how followup simulations can corroborate and improve our understanding of a detected source. Since our method can include all physics provided by full numerical relativity simulations of coalescing binaries, it provides a valuable complement to alternative techniques which employ approximations to reconstruct source parameters. [Preview Abstract] |
Monday, April 18, 2016 3:42PM - 3:54PM |
U14.00002: Reconstructing gravitational wave source parameters via direct comparisons to numerical relativity II: Applications Richard O'Shaughnessy, Jacob Lange, James Healy, Lousto Carlos, Deirdre Shoemaker, Geoffrey Lovelace, Mark Scheel In this talk, we apply a procedure to reconstruct the parameters of sufficiently massive coalescing compact binaries via direct comparison with numerical relativity simulations. We illustrate how to use only comparisons between synthetic data and these simulations to reconstruct properties of a synthetic candidate source. We demonstrate using selected examples that we can reconstruct posterior distributions obtained by other Bayesian methods with our sparse grid. We describe how followup simulations can corroborate and improve our understanding of a candidate signal. [Preview Abstract] |
Monday, April 18, 2016 3:54PM - 4:06PM |
U14.00003: On the measurement of spinning compact binaries with the gravitational-wave observatory Advanced LIGO. Vivien Raymond After years of developments, the Advanced LIGO observatories have completed their first run. This 5-month long record of the gravitational-wave universe is the most sensitive to date, an improvement of several times over the initial instruments. Coalescences of spinning neutron stars and/or black holes are expected to be a main source of gravitational-wave signals, and the extraction of their parameters is especially promising. Spin measurements in particular hold great potential in astrophysical formation scenarios, strong field dynamics, and other fields. In this presentation we report on the spin parameter estimation methods and their applications in the advanced gravitational-wave detector era. [Preview Abstract] |
Monday, April 18, 2016 4:06PM - 4:18PM |
U14.00004: Assessing Accuracy of Waveform Models against Numerical Relativity Waveforms Michael P\"urrer We compare currently available phenomenological and effective-one-body inspiral-merger-ringdown models for gravitational waves (GW) emitted from coalescing black hole binaries against a set of numerical relativity waveforms from the SXS collaboration. Simplifications are used in the construction of some waveform models, such as restriction to spins aligned with the orbital angular momentum, no inclusion of higher harmonics in the GW radiation, no modeling of eccentricity and the use of effective parameters to describe spin precession. In contrast, NR waveforms provide us with a high fidelity representation of the "true" waveform modulo small numerical errors. To focus on systematics we inject NR waveforms into zero noise for early advanced LIGO detector sensitivity at a moderately optimistic signal-to-noise ratio. We discuss where in the parameter space the above modeling assumptions lead to noticeable biases in recovered parameters. [Preview Abstract] |
Monday, April 18, 2016 4:18PM - 4:30PM |
U14.00005: Parameter estimation for inspiraling compact binaries with small orbital eccentricity Marc Favata While most observable inspiraling compact binaries are expected to be nearly circularized, some studies suggest that eccentricity will be non-negligible for a fraction of detectable events. We have recently developed a family of analytic post-Newtonian approximants that incorporate small orbital eccentricity. Using this waveform family we study how well eccentricity and other binary parameters can be measured using ground-based gravitational-wave interferometers. [Preview Abstract] |
Monday, April 18, 2016 4:30PM - 4:42PM |
U14.00006: Parameter estimation and uncertainty for gravitational waves from binary black holes Christopher Berry Binary black holes are one of the most promising sources of gravitational waves that could be observed by Advanced LIGO. To accurately infer the parameters of an astrophysical signal, it is necessary to have a reliable model of the gravitational waveform. Uncertainty in the waveform leads to uncertainty in the measured parameters. For loud signals, this theoretical uncertainty could dominate statistical uncertainty, to be the primary source of error in gravitational-wave astronomy. However, we expect the first candidate events will be closer to the detection threshold. We look at how parameter estimation would be influenced by the use of different waveform models for a binary black-hole signal near detection threshold, and how this can be folded in to a Bayesian analysis. [Preview Abstract] |
Monday, April 18, 2016 4:42PM - 4:54PM |
U14.00007: BayesWave Analysis for LIGO Detector Characterization Joey Shapiro Key The Advanced LIGO gravitational wave detectors successfully collected data during the first observing run (O1) September 2015 to January 2016. The Bayesian inference wavelet decomposition algorithm BayesWave uses a phenomenological parameterized model to characterize the data. Among the BayesWave products are reconstructed waveforms and spectral analysis of instrument noise transients (“glitches”). The BayesWave analysis contributes to our understanding of the LIGO instrument and our ability to distinguish instrument glitches from burst sources of gravitational waves. Preliminary BayesWave analysis of the LIGO O1 data will be presented. [Preview Abstract] |
Monday, April 18, 2016 4:54PM - 5:06PM |
U14.00008: Regression of Environmental and Instrumental Noise in advance LIGO Carlos Filipe Da Silva Costa, Sergey Klimenko, Guenakh V. Mitselmakher The strain sensitivity of advanced LIGO has been improved by a factor three with respect to the initial LIGO. As advanced LIGO is commissioned, the existing noise sources may start to affect its sensitivity and new unexpected environmental and instrumental noise sources may appear. The noise regression method can be used to identify noise sources and subtract noise from the data by using auxiliary channels. I will present the regression method and its applications to the advanced LIGO data. [Preview Abstract] |
Monday, April 18, 2016 5:06PM - 5:18PM |
U14.00009: Tracking down the origins of Advanced LIGO noise: 2 examples Beverly K. Berger For Advanced LIGO to reach design sensitivity various sources of instrumental and environmental noise must be identified and ameliorated. We discuss 2 efforts to search for the origin of noise bursts (glitches) at LIGO Hanford. Advanced LIGO monitors thousands of channels in addition to the gravitational wave channel. These can be studied to find correlations between the gravitational wave channel and other sensor signals. The first type of glitch had a frequency of 50 Hz and a rate of 1 per minute. It was found that the glitches were correlated with ground motion in the end station of the X-arm where the offending air compressor was tracked down and turned off. The second example manifests itself as a sudden, but brief, drop in the range occurring, typically, several times per day at LIGO Hanford and less frequently at LIGO Livingston. These range-drop glitches appear in the gravitational-wave channel. Although correlations with these glitches can be seen in many channels, it cannot be easily determined whether these channels are responding as an effect of this type of very strong glitch or whether they might be related to their cause or causes. To date, the cause of the range-drop glitches is not known. [Preview Abstract] |
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