Reconstructing gravitational wave signals from binary black hole mergers with minimal assumptions
Creators
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1.
Georgia Institute of Technology
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2.
Marshall Space Flight Center
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3.
University of Melbourne
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4.
Montana State University
Abstract
We present a systematic comparison of the binary black hole BBH signal waveform reconstructed by two independent and complementary approaches used in LIGO and Virgo source inference: a template-based analysis and a morphology-independent analysis. We apply the two approaches to real events and to two sets of simulated observations made by adding simulated BBH signals to LIGO and Virgo detector noise. The first set is representative of the ten BBH events in the first gravitational wave transient catalog (GWTC-1). The second set is constructed from a population of BBH systems with total masses and signal strengths in the ranges that ground based detectors are typically sensitive. We find that the reconstruction quality of the GWTC-1 events is consistent with the results of both sets of simulated signals. We also demonstrate a simulated case, where the presence of a mismodeled effect in the observed signal, namely higher order modes, can be identified through the morphology-independent analysis. This study is relevant for currently progressing and future observational runs by LIGO and Virgo.
Additional Information
© 2020 American Physical Society. Received 3 April 2020; accepted 2 September 2020; published 22 September 2020. We would like to thank Christopher Berry and Benjamin Farr for lending us their software packages that we used in injection creation and post processing. We are also grateful to Jonah Kanner and Gregorio Carullo for their valuable comments on the manuscript. This research has made use of data, software and/or web tools obtained from the Gravitational Wave Open Science Center [65], a service of LIGO Laboratory, the LIGO Scientific Collaboration, and the Virgo Collaboration. LIGO is funded by the U.S. National Science Foundation. Virgo is funded by the French Centre National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale della Fisica Nucleare (INFN), and the Dutch Nikhef, with contributions by Polish and Hungarian institutes. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants No. PHY-0757058 and No. PHY-0823459. This research was done using resources provided by the Open Science Grid [66,67], which is supported by the National Science Foundation Grant No. 1148698, and the U.S. Department of Energy's Office of Science. The GT authors gratefully acknowledge the NSF for financial support from Grants No. PHY 1806580, No. PHY 1809572, and No. TG-PHY120016. The Flatiron Institute is supported by the Simons Foundation. Parts of this research were conducted by the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), through Project No. CE170100004. NJC appreciates the support of NSF Grant No. PHY1912053.Attached Files
Published - PhysRevD.102.064056.pdf
Submitted - 2003.09456.pdf
Files
2003.09456.pdf
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Additional details
Identifiers
- Eprint ID
- 104640
- Resolver ID
- CaltechAUTHORS:20200729-131140615
Related works
- Describes
- https://arxiv.org/abs/2003.09456 (URL)
Funding
- Centre National de la Recherche Scientifique (CNRS)
- Istituto Nazionale di Fisica Nucleare (INFN)
- Nikhef
- NSF
- PHY-0757058
- NSF
- PHY-0823459
- NSF
- PHY-1148698
- Department of Energy (DOE)
- NSF
- PHY-1806580
- NSF
- PHY-1809572
- NSF
- TG-PHY120016
- Simons Foundation
- Australian Research Council
- CE170100004
- NSF
- PHY-1912053
Dates
- Created
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2020-07-29Created from EPrint's datestamp field
- Updated
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2022-10-05Created from EPrint's last_modified field