Bulletin of the American Physical Society
APS April Meeting 2021
Volume 66, Number 5
Saturday–Tuesday, April 17–20, 2021; Virtual; Time Zone: Central Daylight Time, USA
Session Y17: Gravitational Wave Data Analysis Methods IILive
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Sponsoring Units: DGRAV Chair: Katerina Chatziioannou, Caltech |
Tuesday, April 20, 2021 1:30PM - 1:42PM Live |
Y17.00001: An All-Sky Search for Continuous Gravitational Waves in the LIGO O3 Data Set Aashish Tripathee The LIGO-Virgo O3 data set offers not only detection of now-familiar compact binary mergers of distant black holes and neutron stars, but potentially the detection of much weaker but continuous radiation from nearby rapidly spinning, non-axisymmetric neutron stars in the galaxy. All-sky searches for such radiation from previously unknown stars using necessarily long data sets are computationally challenging and have given rise to several different approaches. We describe here the application of the well established PowerFlux program, including the method of loose coherence in its outlier followup, to an all-sky search in the first six months of LIGO data from the O3 observing run. The status of the search and its chosen parameters will be presented. [Preview Abstract] |
Tuesday, April 20, 2021 1:42PM - 1:54PM Live |
Y17.00002: Search for continuous gravitational waves from twelve young supernova remnants with a hidden Markov model Margaret Millhouse, Lucy Strang, Andrew Melatos Continuous gravitational waves remain an appealing but as-yet-undiscovered detection prospect in gravitational-wave astronomy. Non-axisymmetric neutron stars may emit continuous gravitational waves at a frequency proportional to their rotation frequency. Continuous waves from rapidly rotating neutron stars, such as those found in some young supernova remnants, may fall in the sensitivity band of the Laser Interferometer Gravitational-Wave Observatory (LIGO). Using a hidden Markov model (HMM) framework, we perform a semi-coherent search for gravitational-wave signals from twelve young supernova remnants in public data from LIGO's second observing run. An HMM is robust to spin-wandering, and can track rapid frequency evolution without explicitly searching over the first derivative of the frequency. This makes the search computationally efficient, and able to search over large stretches of data. [Preview Abstract] |
Tuesday, April 20, 2021 1:54PM - 2:06PM Live |
Y17.00003: Directed searches for continuous gravitational waves Benjamin Owen, Lee Lindblom, Binod Rajbhandari, Luciano Soares Pinheiro I summarize the results of the Texas Tech group's recent searches of publicly available Advanced LIGO data for continuous gravitational waves from the Crab pulsar and from non-pulsing neutron stars in supernova remnants. [Preview Abstract] |
Tuesday, April 20, 2021 2:06PM - 2:18PM Live |
Y17.00004: A Template-based Search for GW190521 and other Intermediate Mass Black Hole Binaries Debnandini Mukherjee GW190521 is the heaviest black hole binary coalescence seen yet with its total mass being about 150 solar masses. In general, intermediate mass black holes (IMBHs) are known to have masses in the range of 100 to 100,000 solar masses and they make up the mass space between the stellar mass and the supermassive black holes. Observation rates of gravitational wave sources with at least one IMBH component, would help constrain their formation channel, which is uncertain at present. In my talk I will discuss the search for sources like GW190521 using pre-computed waveform templates, by executing a matched-filter based search technique known as the GstLAL search. I will also provide an update for the all sky search for IMBHs by GstLAL in the 3rd observing run. [Preview Abstract] |
Tuesday, April 20, 2021 2:18PM - 2:30PM Live |
Y17.00005: Rapid Parameter Estimation of Gravitational Waves from Binary Neutron Star Coalescence using Focused Reduced Order Quadrature Soichiro Morisaki, Vivien Raymond Rapid parameter estimation of gravitational waves from binary neutron star coalescence, in particular accurate sky localization in minutes after the initial detection stage, is crucial for the success of multimessenger observations. One of the techniques to speed up the parameter estimation, which has been applied for the production analysis of the LIGO-Virgo collaboration, is reduced order quadrature (ROQ). While it speeds up parameter estimation significantly, the time required is still on the order of hours. Focusing on the fact that the parameter-estimation follow-up can be tuned with the information available at the detection stage, we improve the ROQ technique and develop a new technique, which we designate focused reduced order quadrature (FROQ). We find that FROQ speeds up the parameter estimation by a factor of $O(10^3)$ to $O(10^4)$ and enables providing accurate source properties such as the location of a source in several tens of minutes after detection. In this talk, we introduce the FROQ technique and show its performance. [Preview Abstract] |
Tuesday, April 20, 2021 2:30PM - 2:42PM Live |
Y17.00006: Fast time-domain waveform model of compact-binary coalescences for LIGO and Virgo observations Deyan Mihaylov, Serguei Ossokine, Alessandra Buonanno We present a computationally efficient time-domain waveform model for spin-aligned compact binary coalescences. The model combines the advantages of the numerical-relativity informed, effective-one-body family of models with a post-adiabatic solution of the equations of motion for the inspiral part of the two-body dynamics. Together with further data-analysis improvements, this enables a new, computationally cheaper way to generate reliable waveforms for compact binaries in the frequency band relevant for LIGO and Virgo. We benchmark this model against other state-of-the-art waveforms in terms of efficiency and accuracy. In particular, we obtain a speed-up of $\sim 10^2$ times for the binary mass range $20 - 100 M_{\odot}$ for the state-of-the-art multipolar EOB waveform model for spin-aligned black holes (SEOBNRv4HM) currently used in LIGO and Virgo observations. [Preview Abstract] |
Tuesday, April 20, 2021 2:42PM - 2:54PM Live |
Y17.00007: The Effect of PSD Drift on the GstLAL PSD Estimator Cody Messick The GstLAL-based inspiral pipeline is one of the LIGO-Virgo-KAGRA matched-filter analyses that searches for gravitational-waves from merging compact binaries. One of the key components of a matched-filtering pipeline is the power spectral density (PSD) estimator. If the PSD changes on timescales smaller than the timescale of the PSD estimate, the signal-to-noise ratio (SNR) can be miscalculated. I will present the GstLAL PSD estimation method and the results of my investigation into the effect of PSD drift on this method. [Preview Abstract] |
Tuesday, April 20, 2021 2:54PM - 3:06PM Live |
Y17.00008: Post-merger gravitational wave searches using the Cross-Correlation Algorithm Tanazza Khanam, Alessandra Corsi, Rob Coyne, Eric Sowell After the multi-messenger detection of the binary neutron star merger GW170817, associated with gamma-ray burst (GRB) 170817a, one big open question left is the nature of the compact remnant which acts as a central engine for the GRB. In the context of cosmological GRBs, it has been suggested that X-ray afterglows showing lightcurve plateaus at timescales of order 10$^{\mathrm{2\thinspace }}$- 10$^{\mathrm{4\thinspace }}$s since the GRB/merger could harbor a long-lived central engine, such as a long-lived highly magnetized NS (magnetar). Newly born magnetars have also been proposed as potential gravitational wave (GW) sources. Motivated by these considerations, we present first results from a new GW data analysis method (the Cross Correlation Algorithm - CoCoA) targeting long-lived GWs from magnetars formed in binary NS mergers associated with GRBs. We show how our search method improves substantially on previously published results for post-merger GW searches in GW170817, but requires a more restrictive hypothesis on the GW signal properties. We conclude by discussing the prospects for these types of searches in future runs of the LIGO detectors. [Preview Abstract] |
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