Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array
We present and evaluate several strategies to search for prompt, low-frequency radio emission associated with gravitational wave transients using the Murchison Widefield Array. As we are able to repoint the Murchison Widefield Array on timescales of tens of seconds, we can search for the dispersed r...
| Main Authors: | , , , , , |
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| Format: | Journal Article |
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Cambridge University Press
2016
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| Online Access: | https://www.cambridge.org/core/services/aop-cambridge-core/content/view/071FE4542A959AEB58527B4339B654A1/S1323358016000436a.pdf/div-class-title-strategies-for-finding-prompt-radio-counterparts-to-gravitational-wave-transients-with-the-murchison-widefield-array-div.pdf http://hdl.handle.net/20.500.11937/27827 |
| _version_ | 1848752371250757632 |
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| author | Kaplan, D. Murphy, T. Rowlinson, A. Croft, S. Wayth, Randall Trott, C. |
| author_facet | Kaplan, D. Murphy, T. Rowlinson, A. Croft, S. Wayth, Randall Trott, C. |
| author_sort | Kaplan, D. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We present and evaluate several strategies to search for prompt, low-frequency radio emission associated with gravitational wave transients using the Murchison Widefield Array. As we are able to repoint the Murchison Widefield Array on timescales of tens of seconds, we can search for the dispersed radio signal that has been predicted to originate along with or shortly after a neutron star-neutron star merger. We find that given the large, 600 deg2 instantaneous field of view of the Murchison Widefield Array, we can cover a significant fraction of the predicted gravitational wave error region, although due to the complicated geometry of the latter, we only cover > 50% of the error region for approximately 5% of events, and roughly 15% of events will be located < 10° from the Murchison Widefield Array pointing centre such that they will be covered in the radio images. For optimal conditions, our limiting flux density for a 10-s long transient would be 0.1 Jy, increasing to about 1 Jy for a wider range of events. This corresponds to luminosity limits of 1038-39 erg s-1 based on expectations for the distances of the gravitational wave transients, which should be sufficient to detect or significantly constrain a range of models for prompt emission. |
| first_indexed | 2025-11-14T08:07:33Z |
| format | Journal Article |
| id | curtin-20.500.11937-27827 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T08:07:33Z |
| publishDate | 2016 |
| publisher | Cambridge University Press |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-278272023-04-26T04:50:09Z Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array Kaplan, D. Murphy, T. Rowlinson, A. Croft, S. Wayth, Randall Trott, C. We present and evaluate several strategies to search for prompt, low-frequency radio emission associated with gravitational wave transients using the Murchison Widefield Array. As we are able to repoint the Murchison Widefield Array on timescales of tens of seconds, we can search for the dispersed radio signal that has been predicted to originate along with or shortly after a neutron star-neutron star merger. We find that given the large, 600 deg2 instantaneous field of view of the Murchison Widefield Array, we can cover a significant fraction of the predicted gravitational wave error region, although due to the complicated geometry of the latter, we only cover > 50% of the error region for approximately 5% of events, and roughly 15% of events will be located < 10° from the Murchison Widefield Array pointing centre such that they will be covered in the radio images. For optimal conditions, our limiting flux density for a 10-s long transient would be 0.1 Jy, increasing to about 1 Jy for a wider range of events. This corresponds to luminosity limits of 1038-39 erg s-1 based on expectations for the distances of the gravitational wave transients, which should be sufficient to detect or significantly constrain a range of models for prompt emission. 2016 Journal Article http://hdl.handle.net/20.500.11937/27827 10.1017/pasa.2016.43 https://www.cambridge.org/core/services/aop-cambridge-core/content/view/071FE4542A959AEB58527B4339B654A1/S1323358016000436a.pdf/div-class-title-strategies-for-finding-prompt-radio-counterparts-to-gravitational-wave-transients-with-the-murchison-widefield-array-div.pdf http://purl.org/au-research/grants/arc/DE140100316 Cambridge University Press unknown |
| spellingShingle | Kaplan, D. Murphy, T. Rowlinson, A. Croft, S. Wayth, Randall Trott, C. Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title | Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title_full | Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title_fullStr | Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title_full_unstemmed | Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title_short | Strategies for Finding Prompt Radio Counterparts to Gravitational Wave Transients with the Murchison Widefield Array |
| title_sort | strategies for finding prompt radio counterparts to gravitational wave transients with the murchison widefield array |
| url | https://www.cambridge.org/core/services/aop-cambridge-core/content/view/071FE4542A959AEB58527B4339B654A1/S1323358016000436a.pdf/div-class-title-strategies-for-finding-prompt-radio-counterparts-to-gravitational-wave-transients-with-the-murchison-widefield-array-div.pdf https://www.cambridge.org/core/services/aop-cambridge-core/content/view/071FE4542A959AEB58527B4339B654A1/S1323358016000436a.pdf/div-class-title-strategies-for-finding-prompt-radio-counterparts-to-gravitational-wave-transients-with-the-murchison-widefield-array-div.pdf http://hdl.handle.net/20.500.11937/27827 |