Bulletin of the American Physical Society
APS April Meeting 2015
Volume 60, Number 4
Saturday–Tuesday, April 11–14, 2015; Baltimore, Maryland
Session C7: Gravitational Wave Data Analysis |
Hide Abstracts |
Sponsoring Units: GGR Chair: Neil Cornish, Montana State University Room: Key 3 |
Saturday, April 11, 2015 1:30PM - 1:42PM |
C7.00001: An analysis of the FrequencyHough method for an all-sky search for continuous gravitational waves Andrew Miller, Pia Astone In this talk we present the Rome-Virgo hierarchical data analysis pipeline for all-sky searches of continuous gravitational wave signals, like those emitted by spinning neutron stars asymmetric with respect to the rotation axis, with unknown position, rotational frequency and spin-down. The core of the pipeline is an incoherent step based on a particularly efficient implementation of the Hough transform, that we call FrequencyHough, that maps the data time/frequency plane to the source frequency/spin-down plane for each fixed direction in the sky. We developed a narrow-band version of the pipeline centered at some reduced parameter space regions, which could be applied to mock data challenge analyses using LIGO or Virgo data. Examples will be shown. [Preview Abstract] |
Saturday, April 11, 2015 1:42PM - 1:54PM |
C7.00002: Observing Gravitational Waves from the Next Nearby Core-Collapse Supernova Sarah Gossan, Christian Ott, Peter Kalmus, Patrick Sutton, Michele Zanolin, Philipp Moesta, Nutsinee Kijbunchoo, Amber Stuver The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on prospective detection scenarios for GWs from CCSNe in the Milky Way, Large Magellanic Cloud, NGC 6822, M31, and M82. We make statements on the detectibility of astrophysically-motivated signals (including waveforms from state-of-the-art 3D CCSN simulations). We utilize real GW detector data, recolored to the predicted noise power spectral densities of the Advanced LIGO (aLIGO) and Advanced Virgo (AdVirgo) detectors at early ($\sim$2015--2017) and late ($\sim$2018--2020) times. We consider various uncertainties in the GW arrival time to investigate sensitivity improvements when arrival time information is provided by neutrino or EM information. [Preview Abstract] |
Saturday, April 11, 2015 1:54PM - 2:06PM |
C7.00003: Constraining Gravitational-Wave Propagation Speed with Multimessenger Observations Atsushi Nishizawa, Takashi Nakamura Detection of gravitational waves (GW) provides us an opportunity to test general relativity in strong and dynamical regimes of gravity. One of the tests is checking whether GW propagates with the speed of light or not. This test is crucial because the velocity of GW has not ever been directly measured. Propagation speed of a GW can deviate from the speed of light due to the modification of gravity, graviton mass, and the nontrivial spacetime structure such as extra dimensions and quantum gravity effects. Here we report a simple method to measure the propagation speed of a GW by directly comparing arrival times between gravitational waves, and neutrinos from supernovae or photons from short gamma-ray bursts. As a result, we found that the future multimessenger observations of a GW, neutrinos, and photons can test the GW propagation speed with the precision of ~$10^{-16}$, improving the previous suggestions by 8-10 orders of magnitude. We also propose a novel method that distinguishes the true signal due to the deviation of GW propagation speed from the speed of light and the intrinsic time delay of the emission at a source by looking at the redshift dependence. [Preview Abstract] |
Saturday, April 11, 2015 2:06PM - 2:18PM |
C7.00004: On Coincidence of Gravitational Waves and Meter-Wavelength Radio Cregg Yancey A case can be built for performing multi-messenger astronomy using gravitational waves and radio for the study of high-energy astrophysical transients. Of key interest are transient events produced by binary neutron star mergers (the primary target), supernovae, and gamma-ray bursts. To this end, this talk will briefly discuss motivations and a proposed method for performing and analyzing coincidence of gravitational-wave and meter-wavelength radio observations to enable multi-messenger astronomy. Additionally, brief discussion is given to the improvement of detection capability for both gravitational-wave and meter-wavelength radio observational instruments through relaxation of detection requirements as a result of coincidence. These improvements are eminently applicable to the near-term target instruments, the Advanced LIGO gravitational-wave detector and the Long-Wavelength Array radio telescope, as well as future observational instruments used in joint observations. [Preview Abstract] |
Saturday, April 11, 2015 2:18PM - 2:30PM |
C7.00005: Measurement of the signal polarization with the network of ground-based gravitational wave detectors Sergey Klimenko Measurement of the gravitational wave (GW) polarization is important for characterization of the wave astrophysical source. In my talk I present a method for reconstruction of the GW signal polarization with networks of GW detectors. The GW polarization state can be visualized as a data pattern in the network plane defined by the antenna pattern vectors. The polarization parameters such as the inclination angle of the source can be extracted from this pattern. I discuss the astrophysical implications of the polarization measurements and the reconstruction capabilities of the existing and future GW detector networks. [Preview Abstract] |
Saturday, April 11, 2015 2:30PM - 2:42PM |
C7.00006: Reconstruction of chirp mass and eccentricity in the search for eccentric binary black holes Vaibhav Tiwari, Sergei Klimenko Eccentric binary black holes are expected to form because of dynamic interaction in the galactic nuclei. A significant fraction of such systems may maintain high eccentricities throughout their lifetime. Gravitational waves (GWs) emitted by these sources have a unique signature and may not be captured efficiently by the searches designed for circular systems. A search for the eccentric binary black holes on the data obtained from GW detectors, LIGO and VIRGO over the S5/S6-VSR1/2/3 run, is being developed using the coherent burst algorithm. The basic premise of the burst search is the detection of un-modeled gravitational wave signals. In the presented talk we describe the reconstruction of the chirp mass and eccentricity from the expected signal signature in the time-frequency domain. The reconstructed parameters are used to constrain the search and improve the search sensitivity. [Preview Abstract] |
Saturday, April 11, 2015 2:42PM - 2:54PM |
C7.00007: Waveform reconstruction with coherent WaveBurst algorithm Claudia Lazzaro, Marco Drago, Sergey Klimenko, Giovanni Andrea Prodi, Maria Concetta Tringali, Gabriele Vedovato The coherent WaveBurst (cWB) algorithm uses a coherent method for detection and reconstruction of transient gravitational wave signals (bursts) by using the constrained likelihood method. The likelihood statistic is built up as a coherent sum over detector responses in the time frequency domain and represents the total signal-to-noise ratio of the GW signal detected in the network. The reconstruction of a GW event by the pipeline includes both the sky location and the signal waveforms. Once the first GW signal is detected, the astrophysical interpretation and the characterization of the emission will depend on the reliability of the waveform reconstruction process. The performances of the pipeline on the reconstruction of the signal parameters is reported. [Preview Abstract] |
Saturday, April 11, 2015 2:54PM - 3:06PM |
C7.00008: Binary Black Holes produced in Globular Clusters Carl Rodriguez, Meagan Morscher, Bharath Pattabiraman, Sourav Chatterjee, Fred Rasio The mergers of binary black holes will be one of the most promising sources for gravitational-wave astronomy; however, the number of sources expected to form dynamically within the dense environments of globular clusters is highly uncertain. We use a Monte Carlo technique to explore the stellar dynamics of globular clusters. This approach can model systems with $\sim 10^6$ stars and realistic stellar physics, enabling the study of even the most massive of galactic globular clusters. We have produced a collection of globular cluster models with structural properties similar to those observed in the Milky Way. We explore the population of binary black holes produced in these models, including the distribution of masses, semi-major axes, and eccentricities. We find that a typical Milky Way globular cluster can produce hundreds of black hole binaries, several tens of which will coalesce within one Hubble time. We use these models to simulate the globular cluster population of a single Milky Way-equivalent galaxy, providing us with the first realistic merger rate of dynamically formed binary black holes in the local universe. [Preview Abstract] |
Saturday, April 11, 2015 3:06PM - 3:18PM |
C7.00009: A comparison of parameterized signal priors for detecting binary black hole mergers Margaret Millhouse, Neil Cornish, Tyson Littenberg In the search for transient gravitational waves, it is believed that modeled template-based searches will be the method of choice for estimating the physical parameters of the gravitational wave producing system. I will discuss an additional method for parameter estimation from burst searches, without having to use a full waveform template. The BayesWave algorithm uses Bayesian inference with a wavelet reconstruction of the gravitational wave signal, and allows for the implementation of a parameterized signal prior which we can use to extract physical quantities such as masses and spins. I will compare two different approaches to developing such a prior, both based on the time-frequency evolution of a binary black hole merger. The first method utilizes a signal prior that favors placing the wavelets along the time-frequency track, while the second method compares the time-frequency track to the time-frequency evolution reconstructed from the waveform produced by BayesWave. [Preview Abstract] |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700