Bulletin of the American Physical Society
APS April Meeting 2013
Volume 58, Number 4
Saturday–Tuesday, April 13–16, 2013; Denver, Colorado
Session G10: Gravitational Wave Data Analysis |
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Sponsoring Units: GGR Chair: Neil Cornish, Montana State University Room: Governor's Square 12 |
Sunday, April 14, 2013 8:30AM - 8:42AM |
G10.00001: BayesWave: a novel method for detecting un-modeled gravitational wave bursts Paul T. Baker, Neil Cornish, Tyson Littenberg The principal challenge of gravitational wave (GW) data analysis is to separate true GW events from non-gaussian noise artifacts. The LIGO-Virgo Burst group has developed several algorithms for detecting un-modeled GW bursts that may be associated with supernova, gamma-ray bursts (GRB), or new physics. These existent algorithms fit for the signals, but do not include explicit models for the non-gaussian detector noise. We describe the BayesWave algorithm, which uses Bayesian model selection techniques to simultaneously fit coherent GW signals across a network of detectors along with non-gaussian and non-stationary noise features, or glitches, in each detector. BayesWave can identify instrument artifacts for detector characterization studies and produce `cleaned' data streams for use by template based searches, such as those for compact binary coalescence. [Preview Abstract] |
Sunday, April 14, 2013 8:42AM - 8:54AM |
G10.00002: Multi-resolution analysis of gravitational-wave signals with the WDM transform Valentin Necula, Sergey Klimenko Searches for transient gravitational wave signals are often performed in the time-frequency domain to identify localized excess power of GW signals. Sensitivity of such (burst) searches improves if the energy of the signal can be captured with a smaller number of the time-frequency components. We present a novel multi-resolution algorithm based on the Wilson-Daubechies-Meyer time-frequency transform which can efficiently represent GW transients with minimal number of time-frequency components and significantly improves the sensitivity of burst searches. [Preview Abstract] |
Sunday, April 14, 2013 8:54AM - 9:06AM |
G10.00003: A Hierarchical Approach to Rapid Gravitational Wave Parameter Estimation Benjamin Farr, Vicky Kalogera The rapid localization of a gravitational wave source is crucial for successfully detecting electromagnetic counterparts. Techniques currently used for analyzing data collected from ground-based detectors assume both objects to be non-spinning, potentially introducing large uncertainties and biases in sky position. Markov Chain Monte Carlo methods have proven capable of estimating the parameters of a fully spinning, circularized compact binaries with high latency, and of rapid sky localization when operating in a lower-dimensional parameter space. We present a technique to connect the two domains, providing rapid yet potentially biased sky localizations within minutes, while slowly increasing the dimensionality of the parameter space in order to account for spin and reduce biases. [Preview Abstract] |
Sunday, April 14, 2013 9:06AM - 9:18AM |
G10.00004: The Application of Bayesian Inference to Gravitational Waves from Core-Collapse Supernovae Sarah Gossan, Christian Ott, Peter Kalmus, Joshua Logue, Siong Heng The gravitational wave (GW) signature of core-collapse supernovae (CCSNe) encodes important information on the supernova explosion mechanism, the workings of which cannot be explored via observations in the electromagnetic spectrum. Recent research has shown that the CCSNe explosion mechanism can be inferred through the application of Bayesian model selection to gravitational wave signals from supernova explosions powered by the neutrino, magnetorotational and acoustic mechanisms. Extending this work, we apply Principal Component Analysis to the GW spectrograms from CCSNe to take into account also the time-frequency evolution of the emitted signals. We do so in the context of Advanced LIGO, to establish if any improvement on distinguishing between various explosion mechanisms can be obtained. Further to this, we consider a five-detector network of interferometers (comprised of the two Advanced LIGO detectors, Advanced Virgo, LIGO India and KAGRA) and generalize the aforementioned analysis for a source of known position but unknown distance, using realistic, re-colored detector data (as opposed to Gaussian noise), in order to make more reliable statements regarding our ability to distinguish between various explosion mechanisms on the basis of their GW signatures. [Preview Abstract] |
Sunday, April 14, 2013 9:18AM - 9:30AM |
G10.00005: Impact of higher-order modes on detecting binary black hole coalescences Larne Pekowsky, James Healy, Pablo Laguna, Deirdre Shoemaker Thus far, modeled searches for the gravitational waves produced by the coalescence of compact binaries have used templates that include only the quadrupolar 2,2 mode. However, it is known that there can be significant power in higher-order modes. In some instances, neglecting these modes could seriously compromise detection. We demonstrate, using numerical relativity waveforms from the late inspiral and merger of binary black holes, how the inclusion of higher modes in a search can increase the sensitivity volume of Advanced LIGO. We also show which higher modes modes are most significant to ensure high sensitivity for systems with un-equal mass and spinning black holes. [Preview Abstract] |
Sunday, April 14, 2013 9:30AM - 9:42AM |
G10.00006: Using a corotating frame to model and interpret gravitational waves from strong-field binary black hole merger Richard O'Shaughnessy, Jim Healy, Larne Pekowsky, Lionel London, Deirdre Shoemaker The short gravitational wave signal from the merger of black hole binaries encodes a surprising amount of information about the strong-field dynamics of merger into frequencies accessible to ground-based interferometers. In this talk we interpret the inspiral, merger, and ringdown signal as ``precession" of the peak emission direction with time. We demonstrate gravitational wave polarization encodes the geometry of precession in an observationally accessible way, both prior to and after merger. In the corotating frame the radiated signal resembles previously-explored nonprecessing systems, with some limitations. [Preview Abstract] |
Sunday, April 14, 2013 9:42AM - 9:54AM |
G10.00007: Gravitational Wave Tests of Strong Field General Relativity with Binary Inspirals: Optimal Model Selection Laura Sampson, Neil Cornish, Nicolas Yunes We study generic tests of strong-field General Relativity with gravitational waves emitted during the inspiral of compact binaries. We construct waveforms that deviate from the General Relativistic expectation through a series of post-Newtonian terms (instead of a single phase term); we find that these higher-order terms can affect our ability to test GR, in some cases by making it easier to detect a deviation, and in some cases by making it more difficult. We find that more complicated, parameterized post-Einsteinian families, with multiple phase terms, are {\emph{suboptimal}} at detecting deviations from General Relativity; the simplest family still reigns supreme when trying to identify whether a deviation from Einstein's theory is present in the data. [Preview Abstract] |
Sunday, April 14, 2013 9:54AM - 10:06AM |
G10.00008: Systematic parameter errors in binary neutron star inspirals: effects of spin, tides, and high post-Newtonian order terms Marc Favata The coalescence of two neutron stars is one of the most important sources for LIGO, Virgo, and other advanced ground-based detectors. Based on a post-Newtonian description of the inspiralling binary, it is generally believed that we will be able to precisely measure the masses of the two neutron stars, and potentially measure (with much less precision) the Love numbers characterizing their tidal distortion (and encoding information about the neutron star radius and equation of state). However, this belief ignores the effects of uncertainties in our knowledge of the waveform. These uncertainties (e.g., the finite order to which we know the post-Newtonian series) can cause a significant systematic offset in the values of the parameters that we extract. I will discuss calculations of these systematic parameter errors for a variety of scenarios. [Preview Abstract] |
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