Method for detection and reconstruction of gravitational wave transients with networks of advanced detectors

By S. Klimenko, G. Vedovato, M. Drago, F. Salemi, V. Tiwari, G. Prodi, C. Lazzaro, K. Ackley, S. Tiwari, C. Silva and 1 more. 2015

277 citations recorded by the source corpus.

We present a method for detection and reconstruction of the gravitational-wave (GW) transients with the networks of advanced detectors. Originally designed to search for transients with the initial GW detectors, it uses signicantly improved algorithms, which enhances both the low-latency searches with rapid localization of GW events for the electro-magnetic followup and high condence detection of a broad range of the transient GW sources. In the paper we present the analytic framework of the method. Following a short description of the core analysis algorithms, we introduce a novel approach to the reconstruction of the GW polarization from a pattern of detector responses to a GW signal. This polarization pattern is a unique signature of an arbitrary GW signal that can be measured independent from the other source parameters. The polarization measurements enable rapid reconstruction of the GW waveforms, sky localization and helps identication of the source origin.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/cde04d220d413aca7d38c43f569885e0c8c54307

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Citations in the corpus

Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo (2013, methodology): “The lowest latency burst sky maps are produced as part of the coherent WaveBurst (cWB) [71, 73] detection pipeline, earlier versions of which were used in prior burst searches [12, 15, 70].”
GWTC-2: Compact Binary Coalescences Observed by LIGO and Virgo During the First Half of the Third Observing Run (2020, methodology): “For each event, the matches are computed between the maximum likelihood template-based waveforms and two minimally modeled waveform reconstruction methods, cWB [112] and BW [107], using data that contain the FIG.”
Tests of general relativity with the binary black hole signals from the LIGO-Virgo catalog GWTC-1 (2019, methodology): “This CWB search [15,39,40] was tuned to detect chirping signals—like those that would be expected from compact binary coalescences—but was not tuned to any specific GR predictions.”
Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo (2019, unknown): “• search-oriented software such as pycbc [149,150], GstLAL [174] and Coherent Waveburst (cWB) [154];”
GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs (2018, methodology): “The signals were discovered using three independent analyses: two matched-filter searches [8,9] and one weakly modeled burst search [11].”
Observation of Gravitational Waves from a Binary Black Hole Merger (2016, unknown): “The initial detection was made by low-latency searches for generic gravitational wave transients [40] and was reported within three minutes of data acquisition [42].”
Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, background): “& Price 2016), LALINFERENCE (Veitch et al. 2015), GSTLAL (Cannon et al. 2012; Privitera et al. 2014), COHERENT WAVEBURST (Klimenko et al. 2016), BAYESWAVE (Cornish & Littenberg 2015), and LALINFERENCEBURST (Veitch et al. 2015).”
The MBTA pipeline for detecting compact binary coalescences in the third LIGO–Virgo observing run (2020, background): “D 98 024050 [13] Q. Chu, PhD Thesis 2017 The University of Western Australia [14] S. Klimenko et al. 2016 Phys.”
Deep Learning for Real-time Gravitational Wave Detection and Parameter Estimation with Advanced LIGO Data (2017, methodology): “y a 3D parameter space (spin-aligned binaries on quasi-circular orbits) [8, 9, 10]—a subset of the over 8D parameter space of GW signals [11, 12, 13, 14]. Extending these searches to target eccentric [15,13,16,17] or spin-precessing BBHs is computationally infeasible [18]. To address these limitatio”