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Transients in the errorbox of GW190814
We are now firmly in the era of multi-messenger astronomy. The detection of the first binary black hole (BBH) merger in GW150914 [1] opened up the era of gravitational wave astronomy, with a further 9 such mergers being detected during the first two observing runs (O1 and O2) of the LIGO Scientific...
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| Format: | Thesis |
| Language: | English |
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Department of Astronomy
2021
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| _version_ | 1867613266931351552 |
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| access_status_str | Open Access |
| author | de Wet, Simon |
| author2 | Groot, Paul J |
| author_browse | Groot, Paul J de Wet, Simon |
| author_facet | Groot, Paul J de Wet, Simon |
| author_sort | de Wet, Simon |
| collection | Thesis |
| description | We are now firmly in the era of multi-messenger astronomy. The detection of the first binary black hole (BBH) merger in GW150914 [1] opened up the era of gravitational wave astronomy, with a further 9 such mergers being detected during the first two observing runs (O1 and O2) of the LIGO Scientific and Virgo Collaborations (LVC). The first – and currently only – multi-messenger source was detected during O2 and was caused by the merger of two neutron stars in a binary system (BNS) [2]. The electromagnetic (EM) counterparts to GW170817 [3] were observed across the EM spectrum by numerous observing facilities, with implications across a vast range of scientific disciplines. Optical/nearinfrared observations demonstrated that the emission was due to a kilonova powered by the radioactive decay of r-process material produced during the merger. For the first time short gamma-ray bursts were convincingly linked to BNS mergers, as observed in GRB170817A [3]. The third LVC observing run (O3) began 2019 April 1 and concluded 2020 March 27. The signal from GW190425 [4] was likely caused by the coalescence of two neutron stars, with the system having a larger total mass than any currently known BNS system. Furthermore, the detection of GW190412 revealed the first BBH merger with a clearly unequal mass ratio of q = m2/m1 = 0.28 along with significant higher-multipole gravitational radiation [5]. |
| format | Thesis |
| id | oai:open.uct.ac.za:11427/32655 |
| institution | University of Cape Town (South Africa) |
| language | eng |
| last_indexed | 2026-06-10T12:33:25.185Z |
| license_str | Not specified — see source repository |
| provenance_str_mv | Harvested via OAI-PMH from UCTD — University of Cape Town Open Access Repository |
| publishDate | 2021 |
| publishDateRange | 2021 |
| publishDateSort | 2021 |
| publisher | Department of Astronomy |
| publisherStr | Department of Astronomy |
| record_format | dspace |
| source_str | UCTD — University of Cape Town Open Access Repository |
| spelling | oai:open.uct.ac.za:11427/32655 Transients in the errorbox of GW190814 de Wet, Simon Groot, Paul J Astronomy We are now firmly in the era of multi-messenger astronomy. The detection of the first binary black hole (BBH) merger in GW150914 [1] opened up the era of gravitational wave astronomy, with a further 9 such mergers being detected during the first two observing runs (O1 and O2) of the LIGO Scientific and Virgo Collaborations (LVC). The first – and currently only – multi-messenger source was detected during O2 and was caused by the merger of two neutron stars in a binary system (BNS) [2]. The electromagnetic (EM) counterparts to GW170817 [3] were observed across the EM spectrum by numerous observing facilities, with implications across a vast range of scientific disciplines. Optical/nearinfrared observations demonstrated that the emission was due to a kilonova powered by the radioactive decay of r-process material produced during the merger. For the first time short gamma-ray bursts were convincingly linked to BNS mergers, as observed in GRB170817A [3]. The third LVC observing run (O3) began 2019 April 1 and concluded 2020 March 27. The signal from GW190425 [4] was likely caused by the coalescence of two neutron stars, with the system having a larger total mass than any currently known BNS system. Furthermore, the detection of GW190412 revealed the first BBH merger with a clearly unequal mass ratio of q = m2/m1 = 0.28 along with significant higher-multipole gravitational radiation [5]. 2021-01-22T07:47:59Z 2021-01-22T07:47:59Z 2020 2021-01-22T06:20:44Z Master Thesis Masters MSc http://hdl.handle.net/11427/32655 eng application/pdf Department of Astronomy Faculty of Science |
| spellingShingle | Astronomy de Wet, Simon Transients in the errorbox of GW190814 |
| thesis_degree_str | Master's |
| title | Transients in the errorbox of GW190814 |
| title_full | Transients in the errorbox of GW190814 |
| title_fullStr | Transients in the errorbox of GW190814 |
| title_full_unstemmed | Transients in the errorbox of GW190814 |
| title_short | Transients in the errorbox of GW190814 |
| title_sort | transients in the errorbox of gw190814 |
| topic | Astronomy |
| url | http://hdl.handle.net/11427/32655 |
| work_keys_str_mv | AT dewetsimon transientsintheerrorboxofgw190814 |