Angular emission patterns of remnant black holes
Abstract
The gravitational radiation from the ringdown of a binary black hole merger is described by the solution of the Teukolsky equation, which predicts both the temporal dependence and the angular distribution of the emission. Many studies have explored the temporal feature of the ringdown wave through black hole spectroscopy. In this work, we further study the spatial distribution, by introducing a global fitting procedure over both temporal and spatial dependencies, to propose a more complete test of general relativity. We show that spin-weighted spheroidal harmonics are the better representation of the ringdown angular emission patterns compared to spin-weighted spherical harmonics. The differences are distinguishable in numerical relativity waveforms. We also study the correlation between progenitor binary properties and the excitation of quasinormal modes, including higher-order angular modes, overtones, prograde, and retrograde modes. Specifically, we show that the excitation of retrograde modes is dominant when the remnant spin is antialigned with the binary orbital angular momentum. This study seeks to provide an analytical strategy and inspire the future development of ringdown tests using real gravitational wave events.
Additional Information
© 2022 American Physical Society. (Received 8 October 2021; accepted 14 December 2021; published 4 January 2022) We thank Sizheng Ma for helpful comments on our selection of waveform from the SXS database. We also thank Sizheng Ma and Keefe Mitman for discussions about the gravitational wave memory effect and BMS frame. We thank Leo Stein, Maximiliano Isi, Katerina Chatziioannou and Geraint Pratten for discussions about ringdown emission. We also thank Arnab Dhani and Bangalore Sathyaprakash for discussions about mirror modes. X. L. and Y. C.'s research is funded by the U.S. National Science Foundation (Grants No. PHY–2011968, No. PHY–2011961, and No. PHY–1836809), the Simons Foundation (Grant No. 568762), and the Brinson Foundation. L. S. and E. P. acknowledge the support of the Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Project No. CE170100004. L. S., R. K. L., and E. P. acknowledge the support of the U.S. National Science Foundation and the LIGO Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the U.S. National Science Foundation and operates under cooperative Agreement No. PHY–1764464. Advanced LIGO was built under Grant No. PHY–0823459. We thank Matthew Giesler for reviewing the manuscript during LIGO PNP.Attached Files
Published - PhysRevD.105.024016.pdf
Accepted Version - 2110.03116.pdf
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Additional details
- Eprint ID
- 112963
- Resolver ID
- CaltechAUTHORS:20220118-839535000
- NSF
- PHY-2011968
- NSF
- PHY-2011961
- NSF
- PHY-1836809
- Simons Foundation
- 568762
- Brinson Foundation
- Australian Research Council
- CE170100004
- NSF
- PHY-1764464
- NSF
- PHY-0823459
- Created
-
2022-01-19Created from EPrint's datestamp field
- Updated
-
2022-01-19Created from EPrint's last_modified field
- Caltech groups
- Walter Burke Institute for Theoretical Physics, LIGO